Author name code: haugan
ADS astronomy entries on 2022-09-14
author:Haugan, S.V.H.
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Title: Euclid: Calibrating photometric redshifts with spectroscopic
cross-correlations
Authors: Naidoo, K.; Johnston, H.; Joachimi, B.; van den Busch,
J. L.; Hildebrandt, H.; Ilbert, O.; Lahav, O.; Aghanim, N.; Altieri,
B.; Amara, A.; Baldi, M.; Bender, R.; Bodendorf, C.; Branchini, E.;
Brescia, M.; Brinchmann, J.; Camera, S.; Capobianco, V.; Carbone,
C.; Carretero, J.; Castander, F. J.; Castellano, M.; Cavuoti, S.;
Cimatti, A.; Cledassou, R.; Congedo, G.; Conselice, C. J.; Conversi,
L.; Copin, Y.; Corcione, L.; Courbin, F.; Cropper, M.; Da Silva, A.;
Degaudenzi, H.; Dinis, J.; Dubath, F.; Dupac, X.; Dusini, S.; Farrens,
S.; Ferriol, S.; Fosalba, P.; Frailis, M.; Franceschi, E.; Franzetti,
P.; Fumana, M.; Galeotta, S.; Garilli, B.; Gillard, W.; Gillis, B.;
Giocoli, C.; Grazian, A.; Grupp, F.; Haugan, S. V. H.; Holmes, W.;
Hormuth, F.; Hornstrup, A.; Jahnke, K.; Kümmel, M.; Kiessling, A.;
Kilbinger, M.; Kitching, T.; Kohley, R.; Kurki-Suonio, H.; Ligori,
S.; Lilje, P. B.; Lloro, I.; Maiorano, E.; Mansutti, O.; Marggraf, O.;
Markovic, K.; Marulli, F.; Massey, R.; Maurogordato, S.; Meneghetti,
M.; Merlin, E.; Meylan, G.; Moresco, M.; Moscardini, L.; Munari, E.;
Nakajima, R.; Niemi, S. M.; Padilla, C.; Paltani, S.; Pasian, F.;
Pedersen, K.; Percival, W. J.; Pettorino, V.; Pires, S.; Polenta, G.;
Poncet, M.; Popa, L.; Pozzetti, L.; Raison, F.; Rebolo, R.; Renzi, A.;
Rhodes, J.; Riccio, G.; Romelli, E.; Rosset, C.; Rossetti, E.; Saglia,
R.; Sapone, D.; Sartoris, B.; Schneider, P.; Secroun, A.; Seidel, G.;
Sirignano, C.; Sirri, G.; Starck, J. -L.; Surace, C.; Tallada-Crespí,
P.; Taylor, A. N.; Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.;
Tutusaus, I.; Valentijn, E. A.; Valenziano, L.; Vassallo, T.; Wang,
Y.; Weller, J.; Wetzstein, M.; Zacchei, A.; Zamorani, G.; Zoubian,
J.; Andreon, S.; Maino, D.; Scottez, V.; Wright, A. H.
Bibcode: 2022arXiv220810503N
Altcode:
Cosmological constraints from key probes of the Euclid imaging survey
rely critically on the accurate determination of the true redshift
distributions $n(z)$ of tomographic redshift bins. We determine
whether the mean redshift $<z>$ of ten Euclid tomographic
redshift bins can be calibrated to the Euclid target uncertainties
of $\sigma(<z>)<0.002\,(1+z)$ via cross-correlation, with
spectroscopic samples akin to those from the Baryon Oscillation
Spectroscopic Survey (BOSS), Dark Energy Spectroscopic Instrument
(DESI), and Euclid's NISP spectroscopic survey. We construct mock
Euclid and spectroscopic galaxy samples from the Flagship simulation
and measure small-scale clustering redshifts up to redshift $z<1.8$
with an algorithm that performs well on current galaxy survey data. The
clustering measurements are then fitted to two $n(z)$ models: one is
the true $n(z)$ with a free mean; the other a Gaussian Process modified
to be restricted to non-negative values. We show that $<z>$
is measured in each tomographic redshift bin to an accuracy of order
0.01 or better. By measuring the clustering redshifts on subsets of
the full Flagship area, we construct scaling relations that allow
us to extrapolate the method performance to larger sky areas than
are currently available in the mock. For the full expected Euclid,
BOSS, and DESI overlap region of approximately 6000 deg$^{2}$, the
uncertainties attainable by clustering redshifts exceeds the Euclid
requirement by at least a factor of three for both $n(z)$ models
considered, although systematic biases limit the accuracy. Clustering
redshifts are an extremely effective method for redshift calibration
for Euclid if the sources of systematic biases can be determined and
removed, or calibrated-out with sufficiently realistic simulations. We
outline possible future work, in particular an extension to higher
redshifts with quasar reference samples.
Title: Euclid preparation. XX. The Complete Calibration of the
Color-Redshift Relation survey: LBT observations and data release
Authors: Euclid Collaboration; Saglia, R.; De Nicola, S.; Fabricius,
M.; Guglielmo, V.; Snigula, J.; Zöller, R.; Bender, R.; Heidt,
J.; Masters, D.; Stern, D.; Paltani, S.; Amara, A.; Auricchio, N.;
Baldi, M.; Bodendorf, C.; Bonino, D.; Branchini, E.; Brescia, M.;
Brinchmann, J.; Camera, S.; Capobianco, V.; Carbone, C.; Carretero, J.;
Castellano, M.; Cavuoti, S.; Cledassou, R.; Congedo, G.; Conselice,
C. J.; Conversi, L.; Copin, Y.; Corcione, L.; Courbin, F.; Cropper,
M.; Da Silva, A.; Degaudenzi, H.; Douspis, M.; Dubath, F.; Duncan,
C. A. J.; Dupac, X.; Dusini, S.; Farrens, S.; Frailis, M.; Franceschi,
E.; Galeotta, S.; Garilli, B.; Gillard, W.; Gillis, B.; Giocoli, C.;
Grazian, A.; Grupp, F.; Haugan, S. V. H.; Hoekstra, H.; Holmes, W.;
Hormuth, F.; Hornstrup, A.; Jahnke, K.; Kümmel, M.; Kermiche, S.;
Kiessling, A.; Kunz, M.; Kurki-Suonio, H.; Laureijs, R.; Ligori, S.;
Lilje, P. B.; Lloro, I.; Maiorano, E.; Marggraf, O.; Markovic, K.;
Marulli, F.; Massey, R.; McCracken, H. J.; Melchior, M.; Meylan, G.;
Moresco, M.; Moscardini, L.; Munari, E.; Niemi, S. M.; Padilla, C.;
Pasian, F.; Pedersen, K.; Percival, W. J.; Pettorino, V.; Pires, S.;
Poncet, M.; Popa, L.; Pozzetti, L.; Raison, F.; Renzi, A.; Rhodes,
J.; Riccio, G.; Romelli, E.; Rossetti, E.; Sapone, D.; Sartoris,
B.; Schneider, P.; Secroun, A.; Seidel, G.; Sirignano, C.; Sirri, G.;
Stanco, L.; Tallada-Crespí, P.; Tavagnacco, D.; Taylor, A. N.; Tereno,
I.; Toledo-Moreo, R.; Torradeflot, F.; Tutusaus, I.; Valentijn, E. A.;
Valenziano, L.; Vassallo, T.; Wang, Y.; Zacchei, A.; Zamorani, G.;
Zoubian, J.; Andreon, S.; Bardelli, S.; Graciá-Carpio, J.; Maino, D.;
Mauri, N.; Tramacere, A.; Zucca, E.; Alvarez Ayllon, A.; Aussel, H.;
Baccigalupi, C.; Balaguera-Antolínez, A.; Ballardini, M.; Biviano,
A.; Bolzonella, M.; Bozzo, E.; Burigana, C.; Cabanac, R.; Cappi, A.;
Carvalho, C. S.; Casas, S.; Castignani, G.; Cooray, A.; Coupon, J.;
Courtois, H. M.; Davini, S.; Desprez, G.; Dole, H.; Escartin, J. A.;
Escoffier, S.; Farina, M.; Fotopoulou, S.; Ganga, K.; Garcia-Bellido,
J.; George, K.; Giacomini, F.; Gozaliasl, G.; Hildebrandt, H.; Hook,
I.; Ilbert, O.; Kansal, V.; Kashlinsky, A.; Keihanen, E.; Kirkpatrick,
C. C.; Loureiro, A.; Macías-Pérez, J.; Magliocchetti, M.; Mainetti,
G.; Maoli, R.; Martinelli, M.; Martinet, N.; Metcalf, R. B.; Morgante,
G.; Nadathur, S.; Nucita, A. A.; Patrizii, L.; Popa, V.; Porciani,
C.; Potter, D.; Pourtsidou, A.; Reimberg, P.; Sánchez, A. G.; Sakr,
Z.; Schirmer, M.; Sefusatti, E.; Sereno, M.; Stadel, J.; Teyssier,
R.; Valieri, C.; Valiviita, J.; Veropalumbo, A.; Viel, M.
Bibcode: 2022A&A...664A.196E
Altcode: 2022arXiv220601620S; 2022arXiv220601620E
The Complete Calibration of the Color-Redshift Relation survey (C3R2)
is a spectroscopic program designed to empirically calibrate the galaxy
color-redshift relation to the Euclid depth (IE = 24.5),
a key ingredient for the success of Stage IV dark energy projects based
on weak lensing cosmology. A spectroscopic calibration sample that is as
representative as possible of the galaxies in the Euclid weak lensing
sample is being collected, selecting galaxies from a self-organizing
map (SOM) representation of the galaxy color space. Here, we present
the results of a near-infrared H- and K-band spectroscopic campaign
carried out using the LUCI instruments at the LBT. For a total of 251
galaxies, we present new highly reliable redshifts in the 1.3 ≤ z
≤ 1.7 and 2 ≤ z ≤ 2.7 ranges. The newly-determined redshifts
populate 49 SOM cells that previously contained no spectroscopic
measurements and almost twice the occupation numbers of an additional
153 SOM cells. A final optical ground-based observational effort is
needed to calibrate the missing cells, in particular in the redshift
range 1.7 ≤ z ≤ 2.7, which lack spectroscopic calibration. In the
end, Euclid itself will deliver telluric-free near-IR spectra that can
complete the calibration. The LBT is an international collaboration
among institutions in the United States, Italy, and Germany. The LBT
Corporation partners are: LBT Beteiligungsgesellschaft, Germany,
representing the Max-Planck Society, the Astrophysical Institute
Potsdam, and Heidelberg University; The University of Arizona on behalf
of the Arizona university system; Istituto Nazionale di Astrofisica,
Italy; The Ohio State University, and The Research Corporation,
on behalf of The University of Notre Dame, University of Minnesota,
and University of Virginia.
Title: Euclid preparation. XXIV. Calibration of the halo mass function
in $\Lambda(\nu)$CDM cosmologies
Authors: Euclid Collaboration; Castro, T.; Fumagalli, A.; Angulo,
R. E.; Bocquet, S.; Borgani, S.; Carbone, C.; Dakin, J.; Dolag,
K.; Giocoli, C.; Monaco, P.; Ragagnin, A.; Saro, A.; Sefusatti,
E.; Costanzi, M.; Amara, A.; Amendola, L.; Baldi, M.; Bender, R.;
Bodendorf, C.; Branchini, E.; Brescia, M.; Camera, S.; Capobianco,
V.; Carretero, J.; Castellano, M.; Cavuoti, S.; Cimatti, A.;
Cledassou, R.; Congedo, G.; Conversi, L.; Copin, Y.; Corcione, L.;
Courbin, F.; Da Silva, A.; Degaudenzi, H.; Douspis, M.; Dubath, F.;
Duncan, C. A. J.; Dupac, X.; Farrens, S.; Ferriol, S.; Fosalba, P.;
Frailis, M.; Franceschi, E.; Galeotta, S.; Garilli, B.; Gillis, B.;
Grazian, A.; Gruppi, F.; Haugan, S. V. H.; Hormuth, F.; Hornstrup,
A.; Hudelot, P.; Jahnke, K.; Kermiche, S.; Kitching, T.; Kunz, M.;
Kurki-Suonio, H.; Lilje, P. B.; Lloro, I.; Mansutti, O.; Marggraf,
O.; Meneghetti, M.; Merlin, E.; Meylan, G.; Moresco, M.; Moscardini,
L.; Munari, E.; Niemi, S. M.; Padilla, C.; Paltani, S.; Pasian, F.;
Pedersen, K.; Pettorino, V.; Pires, S.; Polenta, G.; Poncet, M.;
Popa, L.; Pozzetti, L.; Raison, F.; Rebolo, R.; Renzi, A.; Rhodes,
J.; Riccio, G.; Romelli, E.; Saglia, R.; Sapone, D.; Sartoris, B.;
Schneider, P.; Seidel, G.; Sirri, G.; Stanco, L.; Tallada Crespí,
P.; Taylor, A. N.; Toledo-Moreo, R.; Torradeflot, F.; Tutusaus, I.;
Valentijn, E. A.; Valenziano, L.; Vassallo, T.; Wang, Y.; Weller,
J.; Zacchei, A.; Zamorani, G.; Andreon, S.; Bardelli, S.; Bozzo, E.;
Colodro-Conde, C.; Di Ferdinando, D.; Farina, M.; Graciá-Carpio,
J.; Lindholm, V.; Neissner, C.; Scottez, V.; Tenti, M.; Zucca, E.;
Baccigalupi, C.; Balaguera-Antolínez, A.; Ballardini, M.; Bernardeau,
F.; Biviano, A.; Blanchard, A.; Borlaff, A. S.; Burigana, C.; Cabanac,
R.; Cappi, A.; Carvalho, C. S.; Casas, S.; Castignani, G.; Cooray,
A.; Coupon, J.; Courtois, H. M.; Davini, S.; De Lucia, G.; Desprez,
G.; Dole, H.; Escartin, J. A.; Escoffier, S.; Finelli, F.; Ganga,
K.; Garcia-Bellido, J.; George, K.; Gozaliasl, G.; Hildebrandt, H.;
Hook, I.; Ilić, S.; Kansal, V.; Keihanen, E.; Kirkpatrick, C. C.;
Loureiro, A.; Macias-Perez, J.; Magliocchetti, M.; Maoli, R.; Marcin,
S.; Martinelli, M.; Martinet, N.; Matthew, S.; Maturi, M.; Metcalf,
R. B.; Morgante, G.; Nadathur, S.; Nucita, A. A.; Patrizii, L.; Peel,
A.; Popa, V.; Porciani, C.; Potter, D.; Pourtsidou, A.; Pöntinen, M.;
Sánchez, A. G.; Sakr, Z.; Schirmer, M.; Sereno, M.; Spurio Mancini,
A.; Teyssier, R.; Valiviita, J.; Veropalumbo, A.; Viel, M.
Bibcode: 2022arXiv220802174E
Altcode:
Euclid's photometric galaxy cluster survey has the potential to be
a very competitive cosmological probe. The main cosmological probe
with observations of clusters is their number count, within which the
halo mass function (HMF) is a key theoretical quantity. We present
a new calibration of the analytic HMF, at the level of accuracy
and precision required for the uncertainty in this quantity to be
subdominant with respect to other sources of uncertainty in recovering
cosmological parameters from Euclid cluster counts. Our model is
calibrated against a suite of N-body simulations using a Bayesian
approach taking into account systematic errors arising from numerical
effects in the simulation. First, we test the convergence of HMF
predictions from different N-body codes, by using initial conditions
generated with different orders of Lagrangian Perturbation theory,
and adopting different simulation box sizes and mass resolution. Then,
we quantify the effect of using different halo-finder algorithms,
and how the resulting differences propagate to the cosmological
constraints. In order to trace the violation of universality in
the HMF, we also analyse simulations based on initial conditions
characterised by scale-free power spectra with different spectral
indexes, assuming both Einstein--de Sitter and standard $\Lambda$CDM
expansion histories. Based on these results, we construct a fitting
function for the HMF that we demonstrate to be sub-percent accurate in
reproducing results from 9 different variants of the $\Lambda$CDM model
including massive neutrinos cosmologies. The calibration systematic
uncertainty is largely sub-dominant with respect to the expected
precision of future mass-observation relations; with the only notable
exception of the effect due to the halo finder, that could lead to
biased cosmological inference.
Title: Euclid: Testing the Copernican principle with next-generation
surveys
Authors: Camarena, D.; Marra, V.; Sakr, Z.; Nesseris, S.; Da Silva,
A.; Garcia-Bellido, J.; Fleury, P.; Lombriser, L.; Martinelli, M.;
Martins, C. J. A. P.; Mimoso, J.; Sapone, D.; Clarkson, C.; Camera,
S.; Carbone, C.; Casas, S.; Ilić, S.; Pettorino, V.; Tutusaus,
I.; Aghanim, N.; Altieri, B.; Amara, A.; Auricchio, N.; Baldi, M.;
Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann, J.; Candini, G. P.;
Capobianco, V.; Carretero, J.; Castellano, M.; Cavuoti, S.; Cimatti,
A.; Cledassou, R.; Congedo, G.; Conversi, L.; Copin, Y.; Corcione, L.;
Courbin, F.; Cropper, M.; Degaudenzi, H.; Dubath, F.; Duncan, C. A. J.;
Dupac, X.; Dusini, S.; Ealet, A.; Farrens, S.; Fosalba, P.; Frailis,
M.; Franceschi, E.; Fumana, M.; Garilli, B.; Gillis, B.; Giocoli,
C.; Grazian, A.; Grupp, F.; Haugan, S. V. H.; Holmes, W.; Hormuth,
F.; Hornstrup, A.; Jahnke, K.; Kiessling, A.; Kohley, R.; Kunz, M.;
Kurki-Suonio, H.; Lilje, P. B.; Lloro, I.; Mansutti, O.; Marggraf,
O.; Marulli, F.; Massey, R.; Meneghetti, M.; Merlin, E.; Meylan, G.;
Moresco, M.; Moscardini, L.; Munari, E.; Niemi, S. M.; Padilla, C.;
Paltani, S.; Pasian, F.; Pedersen, K.; Polenta, G.; Poncet, M.; Popa,
L.; Pozzetti, L.; Raison, F.; Rebolo, R.; Rhodes, J.; Riccio, G.;
Rix, Hans-Walter; Rossetti, E.; Saglia, R.; Sartoris, B.; Secroun,
A.; Seidel, G.; Sirignano, C.; Sirri, G.; Stanco, L.; Surace, C.;
Tallada-Crespí, P.; Taylor, A. N.; Tereno, I.; Toledo-Moreo, R.;
Torradeflot, F.; Valentijn, E. A.; Valenziano, L.; Wang, Y.; Zamorani,
G.; Zoubian, J.; Andreon, S.; Di Ferdinando, D.; Scottez, V.; Tenti, M.
Bibcode: 2022arXiv220709995C
Altcode:
The Copernican principle, the notion that we are not at a
special location in the Universe, is one of the cornerstones
of modern cosmology and its violation would invalidate the
Friedmann-Lemaître-Robertson-Walker (FLRW) metric, causing a
major change in our understanding of the Universe. Thus, it is
of fundamental importance to perform observational tests of this
principle. We determine the precision with which future surveys will
be able to test the Copernican principle and their ability to detect
any possible violations. We forecast constraints on the inhomogeneous
Lemaître-Tolman-Bondi model with a cosmological constant $\Lambda$
($\Lambda$LTB), basically a cosmological constant $\Lambda$ and
cold dark matter ($\Lambda$CDM) model, but endowed with a spherical
inhomogeneity. We consider combinations of currently available data and
simulated Euclid data, together with external data products, based on
both $\Lambda$CDM and $\Lambda$LTB fiducial models. These constraints
are compared to the expectations from the Copernican principle. When
considering the $\Lambda$CDM fiducial model, we find that Euclid
data, in combination with other current and forthcoming surveys,
will improve the constraints on the Copernican principle by about
$30\%$, with $\pm10\%$ variations depending on the observables and
scales considered. On the other hand, when considering a $\Lambda$LTB
fiducial model, we find that future Euclid data, combined with other
current and forthcoming data sets, will be able to detect Gpc-scale
inhomogeneities of contrast $-0.1$. Next-generation surveys, such as
Euclid, will thoroughly test homogeneity at large scales, tightening
the constraints on possible violations of the Copernican principle.
Title: Euclid: Forecasts from the void-lensing cross-correlation
Authors: Bonici, M.; Carbone, C.; Vielzeuf, P.; Paganin, L.; Cardone,
V.; Hamaus, N.; Pisani, A.; Hawken, A. J.; Kovacs, A.; Nadathur,
S.; Contarini, S.; Verza, G.; Tutusaus, I.; Marulli, F.; Moscardini,
L.; Aubert, M.; Giocoli, C.; Pourtsidou, A.; Camera, S.; Escoffier,
S.; Caminata, A.; Martinelli, M.; Pallavicini, M.; Pettorino, V.;
Sakr, Z.; Sapone, D.; Testera, G.; Tosi, S.; Yankelevich, V.; Amara,
A.; Auricchio, N.; Baldi, M.; Bonino, D.; Branchini, E.; Brescia,
M.; Brinchmann, J.; Capobianco, V.; Carretero, J.; Castellano, M.;
Cavuoti, S.; Cledassou, R.; Congedo, G.; Conversi, L.; Copin, Y.;
Corcione, L.; Courbin, F.; Cropper, M.; Da Silva, A.; Degaudenzi,
H.; Douspis, M.; Dubath, F.; Duncan, C. A. J.; Dupac, X.; Dusini,
S.; Ealet, A.; Farrens, S.; Ferriol, S.; Fosalba, P.; Frailis, M.;
Franceschi, E.; Fumana, M.; Gomez-Alvarez, P.; Garilli, B.; Gillis,
B.; Grazian, A.; Grupp, F.; Guzzo, L.; Haugan, S. V. H.; Holmes, W.;
Hormuth, F.; Hornstrup, A.; Jahnke, K.; Kummel, M.; Kermiche, S.;
Kiessling, A.; Kilbinger, M.; Kunz, M.; Kurki-Suonio, H.; Laureijs,
R.; Ligori, S.; Lilje, P. B.; Lloro, I.; Maiorano, E.; Mansutti, O.;
Marggraf, O.; Markovic, K.; Massey, R.; Medinaceli, E.; Melchior, M.;
Meneghetti, M.; Meylan, G.; Moresco, M.; Munari, E.; Niemi, S. M.;
Padilla, C.; Paltani, S.; Pasian, F.; Pedersen, K.; Percival, W. J.;
Pires, S.; Polenta, G.; Poncet, M.; Popa, L.; Raison, F.; Rebolo,
R.; Renzi, A.; Rhodes, J.; Rossetti, E.; Saglia, R.; Sartoris, B.;
Scodeggio, M.; Secroun, A.; Seidel, G.; Sirignano, C.; Sirri, G.;
Stanco, L.; Starck, J. -L.; Surace, C.; Tallada-Crespi, P.; Tavagnacco,
D.; Taylor, A. N.; Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.;
Valentijn, E. A.; Valenziano, L.; Wang, Y.; Weller, J.; Zamorani,
G.; Zoubian, J.; Andreon, S.
Bibcode: 2022arXiv220614211B
Altcode:
The Euclid space telescope will survey a large dataset of cosmic
voids traced by dense samples of galaxies. In this work we estimate
its expected performance when exploiting angular photometric void
clustering, galaxy weak lensing and their cross-correlation. To this
aim, we implement a Fisher matrix approach tailored for voids from
the Euclid photometric dataset and present the first forecasts on
cosmological parameters that include the void-lensing correlation. We
examine two different probe settings, pessimistic and optimistic, both
for void clustering and galaxy lensing. We carry out forecast analyses
in four model cosmologies, accounting for a varying total neutrino mass,
$M_\nu$, and a dynamical dark energy (DE) equation of state, $w(z)$,
described by the CPL parametrisation. We find that void clustering
constraints on $h$ and $\Omega_b$ are competitive with galaxy lensing
alone, while errors on $n_s$ decrease thanks to the orthogonality
of the two probes in the 2D-projected parameter space. We also note
that, as a whole, the inclusion of the void-lensing cross-correlation
signal improves parameter constraints by $10-15\%$, and enhances
the joint void clustering and galaxy lensing Figure of Merit (FoM)
by $10\%$ and $25\%$, in the pessimistic and optimistic scenarios,
respectively. Finally, when further combining with the spectroscopic
galaxy clustering, assumed as an independent probe, we find that,
in the most competitive case, the FoM increases by a factor of 4 with
respect to the combination of weak lensing and spectroscopic galaxy
clustering taken as independent probes. The forecasts presented in this
work show that photometric void-clustering and its cross-correlation
with galaxy lensing deserve to be exploited in the data analysis of
the Euclid galaxy survey and promise to improve its constraining power,
especially on $h$, $\Omega_b$, the neutrino mass, and the DE evolution.
Title: Euclid preparation. XVIII. The NISP photometric system
Authors: Euclid Collaboration; Schirmer, M.; Jahnke, K.; Seidel,
G.; Aussel, H.; Bodendorf, C.; Grupp, F.; Hormuth, F.; Wachter,
S.; Appleton, P. N.; Barbier, R.; Brinchmann, J.; Carrasco, J. M.;
Castander, F. J.; Coupon, J.; De Paolis, F.; Franco, A.; Ganga, K.;
Hudelot, P.; Jullo, E.; Lançon, A.; Nucita, A. A.; Paltani, S.;
Smadja, G.; Strafella, F.; Venancio, L. M. G.; Weiler, M.; Amara,
A.; Auphan, T.; Auricchio, N.; Balestra, A.; Bender, R.; Bonino, D.;
Branchini, E.; Brescia, M.; Capobianco, V.; Carbone, C.; Carretero,
J.; Casas, R.; Castellano, M.; Cavuoti, S.; Cimatti, A.; Cledassou,
R.; Congedo, G.; Conselice, C. J.; Conversi, L.; Copin, Y.; Corcione,
L.; Costille, A.; Courbin, F.; Da Silva, A.; Degaudenzi, H.; Douspis,
M.; Dubath, F.; Dupac, X.; Dusini, S.; Ealet, A.; Farrens, S.;
Ferriol, S.; Fosalba, P.; Frailis, M.; Franceschi, E.; Franzetti,
P.; Fumana, M.; Garilli, B.; Gillard, W.; Gillis, B.; Giocoli, C.;
Grazian, A.; Guzzo, L.; Haugan, S. V. H.; Hoekstra, H.; Holmes, W.;
Hornstrup, A.; Kümmel, M.; Kermiche, S.; Kiessling, A.; Kilbinger,
M.; Kitching, T.; Kohley, R.; Kunz, M.; Kurki-Suonio, H.; Laureijs,
R.; Ligori, S.; Lilje, P. B.; Lloro, I.; Maciaszek, T.; Maiorano, E.;
Mansutti, O.; Marggraf, O.; Markovic, K.; Marulli, F.; Massey, R.;
Maurogordato, S.; Mellier, Y.; Meneghetti, M.; Merlin, E.; Meylan,
G.; Moresco, M.; Moscardini, L.; Munari, E.; Nakajima, R.; Nichol,
R. C.; Niemi, S. M.; Padilla, C.; Pasian, F.; Pedersen, K.; Percival,
W. J.; Pettorino, V.; Pires, S.; Poncet, M.; Popa, L.; Pozzetti,
L.; Prieto, E.; Raison, F.; Rhodes, J.; Rix, H. -W.; Roncarelli, M.;
Rossetti, E.; Saglia, R.; Sartoris, B.; Scaramella, R.; Schneider,
P.; Secroun, A.; Serrano, S.; Sirignano, C.; Sirri, G.; Stanco,
L.; Tallada-Crespí, P.; Taylor, A. N.; Teplitz, H. I.; Tereno, I.;
Toledo-Moreo, R.; Torradeflot, F.; Trifoglio, M.; Valentijn, E. A.;
Valenziano, L.; Wang, Y.; Weller, J.; Zamorani, G.; Zoubian, J.;
Andreon, S.; Bardelli, S.; Boucaud, A.; Camera, S.; Farinelli, R.;
Graciá-Carpio, J.; Maino, D.; Medinaceli, E.; Mei, S.; Morisset,
N.; Polenta, G.; Renzi, A.; Romelli, E.; Tenti, M.; Vassallo, T.;
Zacchei, A.; Zucca, E.; Baccigalupi, C.; Balaguera-Antolínez, A.;
Biviano, A.; Blanchard, A.; Borgani, S.; Bozzo, E.; Burigana, C.;
Cabanac, R.; Cappi, A.; Carvalho, C. S.; Casas, S.; Castignani, G.;
Colodro-Conde, C.; Cooray, A. R.; Courtois, H. M.; Crocce, M.; Cuby,
J. -G.; Davini, S.; de la Torre, S.; Di Ferdinando, D.; Escartin,
J. A.; Farina, M.; Ferreira, P. G.; Finelli, F.; Fotopoulou, S.;
Galeotta, S.; Garcia-Bellido, J.; Gaztanaga, E.; George, K.; Gozaliasl,
G.; Hook, I. M.; Ilić, S.; Kansal, V.; Kashlinsky, A.; Keihanen, E.;
Kirkpatrick, C. C.; Lindholm, V.; Mainetti, G.; Maoli, R.; Martinelli,
M.; Martinet, N.; Maturi, M.; Mauri, N.; McCracken, H. J.; Metcalf,
R. B.; Monaco, P.; Morgante, G.; Nightingale, J.; Patrizii, L.; Peel,
A.; Popa, V.; Porciani, C.; Potter, D.; Reimberg, P.; Riccio, G.;
Sánchez, A. G.; Sapone, D.; Scottez, V.; Sefusatti, E.; Teyssier,
R.; Tutusaus, I.; Valieri, C.; Valiviita, J.; Viel, M.; Hildebrandt, H.
Bibcode: 2022A&A...662A..92E
Altcode: 2022arXiv220301650E
Euclid will be the first space mission to survey most of the
extragalactic sky in the 0.95-2.02 µm range, to a 5 σ point-source
median depth of 24.4 AB mag. This unique photometric dataset will
find wide use beyond Euclid's core science. In this paper, we present
accurate computations of the Euclid YE, JE,
and HE passbands used by the Near-Infrared Spectrometer
and Photometer (NISP), and the associated photometric system. We pay
particular attention to passband variations in the field of view,
accounting for, among other factors, spatially variable filter
transmission and variations in the angle of incidence on the filter
substrate using optical ray tracing. The response curves' cut-on
and cut-off wavelengths - and their variation in the field of view -
are determined with ~0.8 nm accuracy, essential for the photometric
redshift accuracy required by Euclid. After computing the photometric
zero points in the AB mag system, we present linear transformations
from and to common ground-based near-infrared photometric systems,
for normal stars, red and brown dwarfs, and galaxies separately. A
Python tool to compute accurate magnitudes for arbitrary passbands and
spectral energy distributions is provided. We discuss various factors,
from space weathering to material outgassing, that may slowly alter
Euclid's spectral response. At the absolute flux scale, the Euclid
in-flight calibration program connects the NISP photometric system
to Hubble Space Telescope spectrophotometric white dwarf standards;
at the relative flux scale, the chromatic evolution of the response
is tracked at the milli-mag level. In this way, we establish an
accurate photometric system that is fully controlled throughout
Euclid's lifetime.
Title: Euclid preparation. XIX. Impact of magnification on photometric
galaxy clustering
Authors: Euclid Collaboration; Lepori, F.; Tutusaus, I.; Viglione,
C.; Bonvin, C.; Camera, S.; Castander, F. J.; Durrer, R.; Fosalba,
P.; Jelic-Cizmek, G.; Kunz, M.; Adamek, J.; Casas, S.; Martinelli,
M.; Sakr, Z.; Sapone, D.; Amara, A.; Auricchio, N.; Bodendorf, C.;
Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann, J.; Capobianco,
V.; Carbone, C.; Carretero, J.; Castellano, M.; Cavuoti, S.; Cimatti,
A.; Cledassou, R.; Congedo, G.; Conselice, C. J.; Conversi, L.;
Copin, Y.; Corcione, L.; Courbin, F.; Da Silva, A.; Degaudenzi, H.;
Douspis, M.; Dubath, F.; Dupac, X.; Dusini, S.; Ealet, A.; Farrens,
S.; Ferriol, S.; Franceschi, E.; Fumana, M.; Garilli, B.; Gillard,
W.; Gillis, B.; Giocoli, C.; Grazian, A.; Grupp, F.; Guzzo, L.;
Haugan, S. V. H.; Holmes, W.; Hormuth, F.; Hudelot, P.; Jahnke, K.;
Kermiche, S.; Kiessling, A.; Kilbinger, M.; Kitching, T.; Kümmel,
M.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro, I.; Mansutti,
O.; Marggraf, O.; Markovic, K.; Marulli, F.; Massey, R.; Maurogordato,
S.; Melchior, M.; Meneghetti, M.; Merlin, E.; Meylan, G.; Moresco, M.;
Moscardini, L.; Munari, E.; Nakajima, R.; Niemi, S. M.; Padilla, C.;
Paltani, S.; Pasian, F.; Pedersen, K.; Percival, W. J.; Pettorino, V.;
Pires, S.; Poncet, M.; Popa, L.; Pozzetti, L.; Raison, F.; Rhodes, J.;
Roncarelli, M.; Rossetti, E.; Saglia, R.; Schneider, P.; Secroun, A.;
Seidel, G.; Serrano, S.; Sirignano, C.; Sirri, G.; Stanco, L.; Starck,
J. -L.; Tallada-Crespí, P.; Taylor, A. N.; Tereno, I.; Toledo-Moreo,
R.; Torradeflot, F.; Valentijn, E. A.; Valenziano, L.; Wang, Y.;
Weller, J.; Zamorani, G.; Zoubian, J.; Andreon, S.; Bardelli, S.;
Fabbian, G.; Graciá-Carpio, J.; Maino, D.; Medinaceli, E.; Mei,
S.; Renzi, A.; Romelli, E.; Sureau, F.; Vassallo, T.; Zacchei, A.;
Zucca, E.; Baccigalupi, C.; Balaguera-Antolínez, A.; Bernardeau, F.;
Biviano, A.; Blanchard, A.; Bolzonella, M.; Borgani, S.; Bozzo, E.;
Burigana, C.; Cabanac, R.; Cappi, A.; Carvalho, C. S.; Castignani, G.;
Colodro-Conde, C.; Coupon, J.; Courtois, H. M.; Cuby, J. -G.; Davini,
S.; de la Torre, S.; Di Ferdinando, D.; Farina, M.; Ferreira, P. G.;
Finelli, F.; Galeotta, S.; Ganga, K.; Garcia-Bellido, J.; Gaztanaga,
E.; Gozaliasl, G.; Hook, I. M.; Ilić, S.; Joachimi, B.; Kansal, V.;
Keihanen, E.; Kirkpatrick, C. C.; Lindholm, V.; Mainetti, G.; Maoli,
R.; Martinet, N.; Maturi, M.; Metcalf, R. B.; Monaco, P.; Morgante,
G.; Nightingale, J.; Nucita, A.; Patrizii, L.; Popa, V.; Potter, D.;
Riccio, G.; Sánchez, A. G.; Schirmer, M.; Schultheis, M.; Scottez, V.;
Sefusatti, E.; Tramacere, A.; Valiviita, J.; Viel, M.; Hildebrandt, H.
Bibcode: 2022A&A...662A..93E
Altcode: 2021arXiv211005435L
Aims: We investigate the importance of lensing magnification for
estimates of galaxy clustering and its cross-correlation with shear
for the photometric sample of Euclid. Using updated specifications,
we study the impact of lensing magnification on the constraints and
the shift in the estimation of the best fitting cosmological parameters
that we expect if this effect is neglected.
Methods: We follow
the prescriptions of the official Euclid Fisher matrix forecast for
the photometric galaxy clustering analysis and the combination of
photometric clustering and cosmic shear. The slope of the luminosity
function (local count slope), which regulates the amplitude of the
lensing magnification, and the galaxy bias have been estimated from the
Euclid Flagship simulation.
Results: We find that magnification
significantly affects both the best-fit estimation of cosmological
parameters and the constraints in the galaxy clustering analysis of
the photometric sample. In particular, including magnification in the
analysis reduces the 1σ errors on Ωm, 0, w0,
wa at the level of 20-35%, depending on how well we will
be able to independently measure the local count slope. In addition,
we find that neglecting magnification in the clustering analysis leads
to shifts of up to 1.6σ in the best-fit parameters. In the joint
analysis of galaxy clustering, cosmic shear, and galaxy-galaxy lensing,
magnification does not improve precision, but it leads to an up to 6σ
bias if neglected. Therefore, for all models considered in this work,
magnification has to be included in the analysis of galaxy clustering
and its cross-correlation with the shear signal (3 × 2pt analysis)
for an accurate parameter estimation.
Title: Euclid preparation: XXIII. Derivation of galaxy physical
properties with deep machine learning using mock fluxes and H-band
images
Authors: Euclid Collaboration; Bisigello, L.; Conselice, C. J.;
Baes, M.; Bolzonella, M.; Brescia, M.; Cavuoti, S.; Cucciati, O.;
Humphrey, A.; Hunt, L. K.; Maraston11, C.; Pozzetti, L.; Tortora, C.;
van Mierlo, S. E.; Aghanim, N.; Auricchio, N.; Baldi, M.; Bender, R.;
Bodendorf, C.; Bonino, D.; Branchini, E.; Brinchmann, J.; Camera,
S.; Capobianco, V.; Carbone, C.; Carretero, J.; Castander, F. J.;
Castellano, M.; Cimatti, A.; Congedo, G.; Conversi, L.; Copin, Y.;
Corcione, L.; Courbin, F.; Cropper, M.; Da Silva, A.; Degaudenzi,
H.; Douspis, M.; Dubath, F.; Duncan, C. A. J.; Dupac, X.; Dusini, S.;
Farrens, S.; Ferriol, S.; Frailis, M.; Franceschi, E.; Franzetti, P.;
Fumana, M.; Garilli, B.; Gillard, W.; Gillis, B.; Giocoli, C.; Grazian,
A.; Grupp, F.; Guzzo, L.; Haugan, S. V. H.; Holmes, W.; Hormuth, F.;
Hornstrup, A.; Jahnke, K.; Kümmel, M.; Kermiche, S.; Kiessling, A.;
Kilbinger, M.; Kohley, R.; Kunz, M.; Kurki-Suonio, H.; Ligori, S.;
Lilje, P. B.; Lloro, I.; Maiorano, E.; Mansutti, O.; Marggraf, O.;
Markovic, K.; Marulli, F.; Massey, R.; Maurogordato, S.; Medinaceli,
E.; Meneghetti, M.; Merlin, E.; Meylan, G.; Moresco, M.; Moscardini,
L.; Munari, E.; Niemi, S. M.; Padilla, C.; Paltani, S.; Pasian,
F.; Pedersen, K.; Pettorino, V.; Polenta, G.; Poncet, M.; Popa, L.;
Raison, F.; Renzi, A.; Rhodes, J.; Riccio, G.; Rix, H. -W.; Romelli,
E.; Roncarelli, M.; Rosset, C.; Rossetti, E.; Saglia, R.; Sapone, D.;
Sartoris, B.; Schneider, P.; Scodeggio, M.; Secroun, A.; Seidel, G.;
Sirignano, C.; Sirri, G.; Stanco, L.; Tallada-Crespí, P.; Tavagnacco,
D.; Taylor, A. N.; Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.;
Tutusaus, I.; Valentijn, E. A.; Valenziano, L.; Vassallo, T.; Wang,
Y.; Zacchei, A.; Zamorani, G.; Zoubian, J.; Andreon, S.; Boucaud,
S. Bardelli A.; Colodro-Conde, C.; Di Ferdinando, D.; Graciá-Carpio,
J.; Lindholm, V.; Maino, D.; Mei, S.; Scottez, V.; Sureau, F.; Tenti,
M.; Zucca, E.; Borlaff, A. S.; Ballardini, M.; Biviano, A.; Bozzo,
E.; Burigana, C.; Cabanac, R.; Cappi, A.; Carvalho, C. S.; Casas,
S.; Castignani, G.; Cooray, A.; Coupon, J.; Courtois, H. M.; Cuby,
J.; Davini, S.; De Lucia, G.; Desprez, G.; Dole, H.; Escartin, J. A.;
Escoffier, S.; Farina, M.; Fotopoulou, S.; Ganga, K.; Garcia-Bellido,
J.; George, K.; Giacomini, F.; Gozaliasl, G.; Hildebrandt, H.; Hook,
I.; Huertas-Company, M.; Kansal, V.; Keihanen, E.; Kirkpatrick, C. C.;
Loureiro, A.; Macías-Pérez, J. F.; Magliocchetti, M.; Mainetti, G.;
Marcin, S.; Martinelli, M.; Martinet, N.; Metcalf, R. B.; Monaco, P.;
Morgante, G.; Nadathur, S.; Nucita, A. A.; Patrizii, L.; Peel, A.;
Potter, D.; Pourtsidou, A.; Pöntinen, M.; Reimberg, P.; Sánchez,
A. G.; Sakr, Z.; Schirmer, M.; Sefusatti, E.; Sereno, M.; Stadel,
J.; Teyssier, R.; Valieri, C.; Valiviita111, J.; Viel, M.
Bibcode: 2022arXiv220614944E
Altcode:
Next generation telescopes, such as Euclid, Rubin/LSST, and Roman,
will open new windows on the Universe, allowing us to infer physical
properties for tens of millions of galaxies. Machine learning methods
are increasingly becoming the most efficient tools to handle this
enormous amount of data, not only as they are faster to apply to data
samples than traditional methods, but because they are also often more
accurate. Properly understanding their applications and limitations
for the exploitation of these data is of utmost importance. In this
paper we present an exploration of this topic by investigating how well
redshifts, stellar masses, and star-formation rates can be measured
with deep learning algorithms for galaxies within data that mimics
the Euclid and Rubin/LSST surveys. We find that Deep Learning Neural
Networks and Convolutional Neutral Networks (CNN), which are dependent
on the parameter space of the sample used for training, perform well in
measuring the properties of these galaxies and have an accuracy which is
better than traditional methods based on spectral energy distribution
fitting. CNNs allow the processing of multi-band magnitudes together
with $H_{E}$-band images. We find that the estimates of stellar
masses improve with the use of an image, but those of redshift and
star-formation rates do not. Our best machine learning results are
deriving i) the redshift within a normalised error of less than 0.15 for
99.9% of the galaxies in the sample with S/N>3 in the $H_{E}$-band;
ii) the stellar mass within a factor of two ($\sim$0.3 dex) for 99.5%
of the considered galaxies; iii) the star-formation rates within a
factor of two ($\sim$0.3 dex) for $\sim$70% of the sample. We discuss
the implications of our work for application to surveys, mainly but
not limited to Euclid and Rubin/LSST, and how measurements of these
galaxy parameters can be improved with deep learning.
Title: Euclid preparation. I. The Euclid Wide Survey
Authors: Euclid Collaboration; Scaramella, R.; Amiaux, J.; Mellier,
Y.; Burigana, C.; Carvalho, C. S.; Cuillandre, J. -C.; Da Silva,
A.; Derosa, A.; Dinis, J.; Maiorano, E.; Maris, M.; Tereno, I.;
Laureijs, R.; Boenke, T.; Buenadicha, G.; Dupac, X.; Gaspar Venancio,
L. M.; Gómez-Álvarez, P.; Hoar, J.; Lorenzo Alvarez, J.; Racca,
G. D.; Saavedra-Criado, G.; Schwartz, J.; Vavrek, R.; Schirmer, M.;
Aussel, H.; Azzollini, R.; Cardone, V. F.; Cropper, M.; Ealet, A.;
Garilli, B.; Gillard, W.; Granett, B. R.; Guzzo, L.; Hoekstra, H.;
Jahnke, K.; Kitching, T.; Maciaszek, T.; Meneghetti, M.; Miller, L.;
Nakajima, R.; Niemi, S. M.; Pasian, F.; Percival, W. J.; Pottinger,
S.; Sauvage, M.; Scodeggio, M.; Wachter, S.; Zacchei, A.; Aghanim,
N.; Amara, A.; Auphan, T.; Auricchio, N.; Awan, S.; Balestra, A.;
Bender, R.; Bodendorf, C.; Bonino, D.; Branchini, E.; Brau-Nogue, S.;
Brescia, M.; Candini, G. P.; Capobianco, V.; Carbone, C.; Carlberg,
R. G.; Carretero, J.; Casas, R.; Castander, F. J.; Castellano, M.;
Cavuoti, S.; Cimatti, A.; Cledassou, R.; Congedo, G.; Conselice,
C. J.; Conversi, L.; Copin, Y.; Corcione, L.; Costille, A.; Courbin,
F.; Degaudenzi, H.; Douspis, M.; Dubath, F.; Duncan, C. A. J.; Dusini,
S.; Farrens, S.; Ferriol, S.; Fosalba, P.; Fourmanoit, N.; Frailis,
M.; Franceschi, E.; Franzetti, P.; Fumana, M.; Gillis, B.; Giocoli,
C.; Grazian, A.; Grupp, F.; Haugan, S. V. H.; Holmes, W.; Hormuth, F.;
Hudelot, P.; Kermiche, S.; Kiessling, A.; Kilbinger, M.; Kohley, R.;
Kubik, B.; Kümmel, M.; Kunz, M.; Kurki-Suonio, H.; Lahav, O.; Ligori,
S.; Lilje, P. B.; Lloro, I.; Mansutti, O.; Marggraf, O.; Markovic,
K.; Marulli, F.; Massey, R.; Maurogordato, S.; Melchior, M.; Merlin,
E.; Meylan, G.; Mohr, J. J.; Moresco, M.; Morin, B.; Moscardini,
L.; Munari, E.; Nichol, R. C.; Padilla, C.; Paltani, S.; Peacock, J.;
Pedersen, K.; Pettorino, V.; Pires, S.; Poncet, M.; Popa, L.; Pozzetti,
L.; Raison, F.; Rebolo, R.; Rhodes, J.; Rix, H. -W.; Roncarelli, M.;
Rossetti, E.; Saglia, R.; Schneider, P.; Schrabback, T.; Secroun,
A.; Seidel, G.; Serrano, S.; Sirignano, C.; Sirri, G.; Skottfelt,
J.; Stanco, L.; Starck, J. L.; Tallada-Crespí, P.; Tavagnacco, D.;
Taylor, A. N.; Teplitz, H. I.; Toledo-Moreo, R.; Torradeflot, F.;
Trifoglio, M.; Valentijn, E. A.; Valenziano, L.; Verdoes Kleijn,
G. A.; Wang, Y.; Welikala, N.; Weller, J.; Wetzstein, M.; Zamorani,
G.; Zoubian, J.; Andreon, S.; Baldi, M.; Bardelli, S.; Boucaud, A.;
Camera, S.; Di Ferdinando, D.; Fabbian, G.; Farinelli, R.; Galeotta,
S.; Graciá-Carpio, J.; Maino, D.; Medinaceli, E.; Mei, S.; Neissner,
C.; Polenta, G.; Renzi, A.; Romelli, E.; Rosset, C.; Sureau, F.; Tenti,
M.; Vassallo, T.; Zucca, E.; Baccigalupi, C.; Balaguera-Antolínez,
A.; Battaglia, P.; Biviano, A.; Borgani, S.; Bozzo, E.; Cabanac,
R.; Cappi, A.; Casas, S.; Castignani, G.; Colodro-Conde, C.;
Coupon, J.; Courtois, H. M.; Cuby, J.; de la Torre, S.; Desai, S.;
Dole, H.; Fabricius, M.; Farina, M.; Ferreira, P. G.; Finelli, F.;
Flose-Reimberg, P.; Fotopoulou, S.; Ganga, K.; Gozaliasl, G.; Hook,
I. M.; Keihanen, E.; Kirkpatrick, C. C.; Liebing, P.; Lindholm, V.;
Mainetti, G.; Martinelli, M.; Martinet, N.; Maturi, M.; McCracken,
H. J.; Metcalf, R. B.; Morgante, G.; Nightingale, J.; Nucita, A.;
Patrizii, L.; Potter, D.; Riccio, G.; Sánchez, A. G.; Sapone, D.;
Schewtschenko, J. A.; Schultheis, M.; Scottez, V.; Teyssier, R.;
Tutusaus, I.; Valiviita, J.; Viel, M.; Vriend, W.; Whittaker, L.
Bibcode: 2022A&A...662A.112E
Altcode: 2021arXiv210801201S
Euclid is a mission of the European Space Agency that is designed
to constrain the properties of dark energy and gravity via weak
gravitational lensing and galaxy clustering. It will carry out a wide
area imaging and spectroscopy survey (the Euclid Wide Survey: EWS)
in visible and near-infrared bands, covering approximately 15 000
deg2 of extragalactic sky in six years. The wide-field
telescope and instruments are optimised for pristine point spread
function and reduced stray light, producing very crisp images. This
paper presents the building of the Euclid reference survey: the
sequence of pointings of EWS, deep fields, and calibration fields,
as well as spacecraft movements followed by Euclid as it operates in a
step-and-stare mode from its orbit around the Lagrange point L2. Each
EWS pointing has four dithered frames; we simulated the dither pattern
at the pixel level to analyse the effective coverage. We used up-to-date
models for the sky background to define the Euclid region-of-interest
(RoI). The building of the reference survey is highly constrained from
calibration cadences, spacecraft constraints, and background levels;
synergies with ground-based coverage were also considered. Via purposely
built software, we first generated a schedule for the calibrations
and deep fields observations. On a second stage, the RoI was tiled
and scheduled with EWS observations, using an algorithm optimised
to prioritise the best sky areas, produce a compact coverage, and
ensure thermal stability. The result is the optimised reference survey
RSD_2021A, which fulfils all constraints and is a good proxy for the
final solution. The current EWS covers ≈14 500 deg2. The
limiting AB magnitudes (5σ point-like source) achieved in its footprint
are estimated to be 26.2 (visible band IE) and 24.5 (for
near infrared bands YE, JE, HE);
for spectroscopy, the Hα line flux limit is 2 × 10−16
erg−1 cm−2 s−1 at 1600 nm;
and for diffuse emission, the surface brightness limits are 29.8
(visible band) and 28.4 (near infrared bands) mag arcsec−2.
Title: Euclid: Fast two-point correlation function covariance through
linear construction
Authors: Keihanen, E.; Lindholm, V.; Monaco, P.; Blot, L.; Carbone,
C.; Kiiveri, K.; Sánchez, A. G.; Viitanen, A.; Valiviita, J.; Amara,
A.; Auricchio, N.; Baldi, M.; Bonino, D.; Branchini, E.; Brescia, M.;
Brinchmann, J.; Camera, S.; Capobianco, V.; Carretero, J.; Castellano,
M.; Cavuoti, S.; Cimatti, A.; Cledassou, R.; Congedo, G.; Conversi,
L.; Copin, Y.; Corcione, L.; Cropper, M.; Da Silva, A.; Degaudenzi,
H.; Douspis, M.; Dubath, F.; Duncan, C. A. J.; Dupac, X.; Dusini,
S.; Ealet, A.; Farrens, S.; Ferriol, S.; Frailis, M.; Franceschi, E.;
Fumana, M.; Gillis, B.; Giocoli, C.; Grazian, A.; Grupp, F.; Guzzo,
L.; Haugan, S. V. H.; Hoekstra, H.; Holmes, W.; Hormuth, F.; Jahnke,
K.; Kümmel, M.; Kermiche, S.; Kiessling, A.; Kitching, T.; Kunz,
M.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro, I.; Maiorano,
E.; Mansutti, O.; Marggraf, O.; Marulli, F.; Massey, R.; Melchior,
M.; Meneghetti, M.; Meylan, G.; Moresco, M.; Morin, B.; Moscardini,
L.; Munari, E.; Niemi, S. M.; Padilla, C.; Paltani, S.; Pasian, F.;
Pedersen, K.; Pettorino, V.; Pires, S.; Polenta, G.; Poncet, M.;
Popa, L.; Raison, F.; Renzi, A.; Rhodes, J.; Romelli, E.; Saglia, R.;
Sartoris, B.; Schneider, P.; Schrabback, T.; Secroun, A.; Seidel, G.;
Sirignano, C.; Sirri, G.; Stanco, L.; Surace, C.; Tallada-Crespí,
P.; Tavagnacco, D.; Taylor, A. N.; Tereno, I.; Toledo-Moreo, R.;
Torradeflot, F.; Valentijn, E. A.; Valenziano, L.; Vassallo, T.;
Wang, Y.; Weller, J.; Zamorani, G.; Zoubian, J.; Andreon, S.; Maino,
D.; de la Torre, S.
Bibcode: 2022arXiv220511852K
Altcode:
We present a method for fast evaluation of the covariance matrix
for a two-point galaxy correlation function (2PCF) measured with
the Landy-Szalay estimator. The standard way of evaluating the
covariance matrix consists in running the estimator on a large number
of mock catalogs, and evaluating their sample covariance. With large
random catalog sizes (data-to-random objects ratio M>>1) the
computational cost of the standard method is dominated by that of
counting the data-random and random-random pairs, while the uncertainty
of the estimate is dominated by that of data-data pairs. We present
a method called Linear Construction (LC), where the covariance is
estimated for small random catalogs of size M = 1 and M = 2, and the
covariance for arbitrary M is constructed as a linear combination of
these. We validate the method with PINOCCHIO simulations in range r =
20-200 Mpc/h, and show that the covariance estimate is unbiased. With
M = 50 and with 2 Mpc/h bins, the theoretical speed-up of the method
is a factor of 14. We discuss the impact on the precision matrix
and parameter estimation, and derive a formula for the covariance
of covariance.
Title: Euclid preparation: XXI. Intermediate-redshift contaminants
in the search for $z>6$ galaxies within the Euclid Deep Survey
Authors: Euclid Collaboration; van Mierlo, S. E.; Caputi, K. I.;
Ashby, M.; Atek, H.; Bolzonella, M.; Bowler, R. A. A.; Brammer,
G.; Conselice, C. J.; Cuby, J.; Dayal, P.; Díaz-Sánchez, A.;
Finkelstein, S. L.; Hoekstra, H.; Humphrey, A.; Ilbert, O.; McCracken,
H. J.; Milvang-Jensen, B.; Oesch, P. A.; Pello, R.; Rodighiero,
G.; Schirmer, M.; Toft, S.; Weaver, J. R.; Wilkins, S. M.; Willott,
C. J.; Zamorani, G.; Amara, A.; Auricchio, N.; Baldi, M.; Bender, R.;
Bodendorf, C.; Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann, J.;
Camera, S.; Capobianco, V.; Carbone, C.; Carretero, J.; Castellano,
M.; Cavuoti, S.; Cimatti, A.; Cledassou, R.; Congedo, G.; Conversi,
L.; Copin, Y.; Corcione, L.; Courbin, F.; Da Silva, A.; Degaudenzi,
H.; Douspis, M.; Dubath, F.; Dupac, X.; Dusini, S.; Farrens, S.;
Ferriol, S.; Frailis, M.; Franceschi, E.; Franzetti, P.; Fumana,
M.; Galeotta, S.; Garilli, B.; Gillard, W.; Gillis, B.; Giocoli, C.;
Grazian, A.; Grupp, F.; Haugan, S. V. H.; Holmes, W.; Hormuth, F.;
Hornstrup, A.; Jahnke, K.; Kümmel, M.; Kiessling, A.; Kilbinger,
M.; Kitching, T.; Kohley, R.; Kunz, M.; Kurki-Suonio, H.; Laureijs,
R.; Ligori, S.; Lilje, P. B.; Lloro, I.; Maiorano, E.; Mansutti, O.;
Marggraf, O.; Markovic, K.; Marulli, F.; Massey, R.; Maurogordato,
S.; Medinaceli, E.; Meneghetti, M.; Merlin, E.; Meylan, G.; Moresco,
M.; Moscardini, L.; Munari, E.; Niemi, S. M.; Padilla, C.; Paltani,
S.; Pasian, F.; Pedersen, K.; Pettorino, V.; Pires, S.; Poncet, M.;
Popa, L.; Pozzetti, L.; Raison, F.; Renzi, A.; Rhodes, J.; Riccio,
G.; Romelli, E.; Rossetti, E.; Saglia, R.; Sapone, D.; Sartoris,
B.; Schneider, P.; Secroun, A.; Sirignano, C.; Sirri, G.; Stanco,
L.; Starck, J. -L.; Surace, C.; Tallada-Crespí, P.; Taylor, A. N.;
Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.; Tutusaus, I.; Valentijn,
E. A.; Valenziano, L.; Vassallo, T.; Wang, Y.; Zacchei, A.; Zoubian,
J.; Andreon, S.; Bardelli, S.; Boucaud, A.; Graciá-Carpio, J.;
Maino, D.; Mauri, N.; Mei, S.; Sureau, F.; Zucca, E.; Aussel, H.;
Baccigalupi, C.; Balaguera-Antolínez, A.; Biviano, A.; Blanchard,
A.; Borgani, S.; Bozzo, E.; Burigana, C.; Cabanac, R.; Calura, F.;
Cappi, A.; Carvalho, C. S.; Casas, S.; Castignani, G.; Colodro-Conde,
C.; Cooray, A. R.; Coupon, J.; Courtois, H. M.; Crocce, M.; Cucciati,
O.; Davini, S.; Dole, H.; Escartin, J. A.; Escoffier, S.; Fabricius,
M.; Farina, M.; Ganga, K.; García-Bellido, J.; George, K.; Giacomini,
F.; Gozaliasl, G.; Gwyn, S.; Hook, I.; Huertas-Company, M.; Kansal,
V.; Kashlinsky, A.; Keihanen, E.; Kirkpatrick, C. C.; Lindholm,
V.; Maoli, R.; Martinelli, M.; Martinet, N.; Maturi, M.; Metcalf,
R. B.; Monaco, P.; Morgante, G.; Nucita, A. A.; Patrizii, L.; Peel,
A.; Pollack, J.; Popa, V.; Porciani, C.; Potter, D.; Reimberg, P.;
Sánchez, A. G.; Scottez, V.; Sefusatti, E.; Stadel, J.; Teyssier,
R.; Valiviita, J.; Viel, M.
Bibcode: 2022arXiv220502871E
Altcode:
(Abridged) The Euclid mission is expected to discover thousands of
z>6 galaxies in three Deep Fields, which together will cover a ~40
deg2 area. However, the limited number of Euclid bands and availability
of ancillary data could make the identification of z>6 galaxies
challenging. In this work, we assess the degree of contamination by
intermediate-redshift galaxies (z=1-5.8) expected for z>6 galaxies
within the Euclid Deep Survey. This study is based on ~176,000 real
galaxies at z=1-8 in a ~0.7 deg2 area selected from the UltraVISTA
ultra-deep survey, and ~96,000 mock galaxies with 25.3$\leq$H<27.0,
which altogether cover the range of magnitudes to be probed in the
Euclid Deep Survey. We simulate Euclid and ancillary photometry from
the fiducial, 28-band photometry, and fit spectral energy distributions
(SEDs) to various combinations of these simulated data. Our study
demonstrates that identifying z>6 with Euclid data alone will be
very effective, with a z>6 recovery of 91(88)% for bright (faint)
galaxies. For the UltraVISTA-like bright sample, the percentage of
z=1-5.8 contaminants amongst apparent z>6 galaxies as observed with
Euclid alone is 18%, which is reduced to 4(13)% by including ultra-deep
Rubin (Spitzer) photometry. Conversely, for the faint mock sample,
the contamination fraction with Euclid alone is considerably higher
at 39%, and minimized to 7% when including ultra-deep Rubin data. For
UltraVISTA-like bright galaxies, we find that Euclid (I-Y)>2.8 and
(Y-J)<1.4 colour criteria can separate contaminants from true
z>6 galaxies, although these are applicable to only 54% of the
contaminants, as many have unconstrained (I-Y) colours. In the most
optimistic scenario, these cuts reduce the contamination fraction to
1% whilst preserving 81% of the fiducial z>6 sample. For the faint
mock sample, colour cuts are infeasible.
Title: Euclid: Cosmological forecasts from the void size function
Authors: Contarini, S.; Verza, G.; Pisani, A.; Hamaus, N.; Sahlén,
M.; Carbone, C.; Dusini, S.; Marulli, F.; Moscardini, L.; Renzi, A.;
Sirignano, C.; Stanco, L.; Aubert, M.; Bonici, M.; Castignani, G.;
Courtois, H. M.; Escoffier, S.; Guinet, D.; Kovacs, A.; Lavaux, G.;
Massara, E.; Nadathur, S.; Pollina, G.; Ronconi, T.; Ruppin, F.; Sakr,
Z.; Veropalumbo, A.; Wandelt, B. D.; Amara, A.; Auricchio, N.; Baldi,
M.; Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann, J.; Camera, S.;
Capobianco, V.; Carretero, J.; Castellano, M.; Cavuoti, S.; Cledassou,
R.; Congedo, G.; Conselice, C. J.; Conversi, L.; Copin, Y.; Corcione,
L.; Courbin, F.; Cropper, M.; Da Silva, A.; Degaudenzi, H.; Dubath,
F.; Duncan, C. A. J.; Dupac, X.; Ealet, A.; Farrens, S.; Ferriol, S.;
Fosalba, P.; Frailis, M.; Franceschi, E.; Garilli, B.; Gillard, W.;
Gillis, B.; Giocoli, C.; Grazian, A.; Grupp, F.; Guzzo, L.; Haugan,
S.; Holmes, W.; Hormuth, F.; Jahnke, K.; Kümmel, M.; Kermiche, S.;
Kiessling, A.; Kilbinger, M.; Kunz, M.; Kurki-Suonio, H.; Laureijs,
R.; Ligori, S.; Lilje, P. B.; Lloro, I.; Maiorano, E.; Mansutti, O.;
Marggraf, O.; Markovic, K.; Massey, R.; Melchior, M.; Meneghetti,
M.; Meylan, G.; Moresco, M.; Munari, E.; Niemi, S. M.; Padilla, C.;
Paltani, S.; Pasian, F.; Pedersen, K.; Percival, W. J.; Pettorino, V.;
Pires, S.; Polenta, G.; Poncet, M.; Popa, L.; Pozzetti, L.; Raison,
F.; Rhodes, J.; Rossetti, E.; Saglia, R.; Sartoris, B.; Schneider,
P.; Secroun, A.; Seidel, G.; Sirri, G.; Surace, C.; Tallada-Crespí,
P.; Taylor, A. N.; Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.;
Valentijn, E. A.; Valenziano, L.; Wang, Y.; Weller, J.; Zamorani,
G.; Zoubian, J.; Andreon, S.; Maino, D.; Mei, S.
Bibcode: 2022arXiv220511525C
Altcode:
The Euclid mission $-$ with its spectroscopic galaxy survey covering
a sky area over $15\,000 \ \mathrm{deg}^2$ in the redshift range
$0.9<z<1.8\ -$ will provide a sample of tens of thousands of
cosmic voids. This paper explores for the first time the constraining
power of the void size function on the properties of dark energy
(DE) from a survey mock catalogue, the official Euclid Flagship
simulation. We identify voids in the Flagship light-cone, which
closely matches the features of the upcoming Euclid spectroscopic
data set. We model the void size function considering a state-of-the
art methodology: we rely on the volume conserving (Vdn) model,
a modification of the popular Sheth & van de Weygaert model
for void number counts, extended by means of a linear function of
the large-scale galaxy bias. We find an excellent agreement between
model predictions and measured mock void number counts. We compute
updated forecasts for the Euclid mission on DE from the void size
function and provide reliable void number estimates to serve as
a basis for further forecasts of cosmological applications using
voids. We analyse two different cosmological models for DE: the
first described by a constant DE equation of state parameter, $w$,
and the second by a dynamic equation of state with coefficients $w_0$
and $w_a$. We forecast $1\sigma$ errors on $w$ lower than the $10\%$,
and we estimate an expected figure of merit (FoM) for the dynamical
DE scenario $\mathrm{FoM}_{w_0,w_a} = 17$ when considering only the
neutrino mass as additional free parameter of the model. The analysis
is based on conservative assumptions to ensure full robustness, and
is a pathfinder for future enhancements of the technique. Our results
showcase the impressive constraining power of the void size function
from the Euclid spectroscopic sample, both as a stand-alone probe,
and to be combined with other Euclid cosmological probes.
Title: Euclid: Constraining ensemble photometric redshift
distributions with stacked spectroscopy
Authors: Cagliari, M. S.; Granett, B. R.; Guzzo, L.; Bolzonella,
M.; Pozzetti, L.; Tutusaus, I.; Camera, S.; Amara, A.; Auricchio,
N.; Bender, R.; Bodendorf, C.; Bonino, D.; Branchini, E.; Brescia,
M.; Capobianco, V.; Carbone, C.; Carretero, J.; Castander, F. J.;
Castellano, M.; Cavuoti, S.; Cimatti, A.; Cledassou, R.; Congedo,
G.; Conselice, C. J.; Conversi, L.; Copin, Y.; Corcione, L.; Cropper,
M.; Degaudenzi, H.; Douspis, M.; Dubath, F.; Dusini, S.; Ealet, A.;
Ferriol, S.; Fourmanoit, N.; Frailis, M.; Franceschi, E.; Franzetti,
P.; Garilli, B.; Giocoli, C.; Grazian, A.; Grupp, F.; Haugan, S. V. H.;
Hoekstra, H.; Holmes, W.; Hormuth, F.; Hudelot, P.; Jahnke, K.;
Kermiche, S.; Kiessling, A.; Kilbinger, M.; Kitching, T.; Kümmel,
M.; Kunz, M.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro, I.;
Maiorano, E.; Mansutti, O.; Marggraf, O.; Markovic, K.; Massey, R.;
Meneghetti, M.; Merlin, E.; Meylan, G.; Moresco, M.; Moscardini,
L.; Niemi, S. M.; Padilla, C.; Paltani, S.; Pasian, F.; Pedersen,
K.; Percival, W. J.; Pettorino, V.; Pires, S.; Poncet, M.; Popa,
L.; Raison, F.; Rebolo, R.; Rhodes, J.; Rix, H. -W.; Roncarelli, M.;
Rossetti, E.; Saglia, R.; Scaramella, R.; Schneider, P.; Scodeggio,
M.; Secroun, A.; Seidel, G.; Serrano, S.; Sirignano, C.; Sirri, G.;
Tavagnacco, D.; Taylor, A. N.; Tereno, I.; Toledo-Moreo, R.; Valentijn,
E. A.; Valenziano, L.; Wang, Y.; Welikala, N.; Weller, J.; Zamorani,
G.; Zoubian, J.; Baldi, M.; Farinelli, R.; Medinaceli, E.; Mei, S.;
Polenta, G.; Romelli, E.; Vassallo, T.; Humphrey, A.
Bibcode: 2022A&A...660A...9C
Altcode: 2021arXiv210907303C
Context. The ESA Euclid mission will produce photometric galaxy
samples over 15 000 square degrees of the sky that will be rich for
clustering and weak lensing statistics. The accuracy of the cosmological
constraints derived from these measurements will depend on the knowledge
of the underlying redshift distributions based on photometric redshift
calibrations.
Aims: A new approach is proposed to use the
stacked spectra from Euclid slitless spectroscopy to augment broad-band
photometric information to constrain the redshift distribution with
spectral energy distribution fitting. The high spectral resolution
available in the stacked spectra complements the photometry and helps
to break the colour-redshift degeneracy and constrain the redshift
distribution of galaxy samples.
Methods: We modelled the stacked
spectra as a linear mixture of spectral templates. The mixture may be
inverted to infer the underlying redshift distribution using constrained
regression algorithms. We demonstrate the method on simulated Vera
C. Rubin Observatory and Euclid mock survey data sets based on the
Euclid Flagship mock galaxy catalogue. We assess the accuracy of the
reconstruction by considering the inference of the baryon acoustic
scale from angular two-point correlation function measurements.
Results: We selected mock photometric galaxy samples at redshift z >
1 using the self-organising map algorithm. Considering the idealised
case without dust attenuation, we find that the redshift distributions
of these samples can be recovered with 0.5% accuracy on the baryon
acoustic scale. The estimates are not significantly degraded by the
spectroscopic measurement noise due to the large sample size. However,
the error degrades to 2% when the dust attenuation model is left
free. We find that the colour degeneracies introduced by attenuation
limit the accuracy considering the wavelength coverage of Euclid
near-infrared spectroscopy. This paper is published on behalf of
the Euclid Consortium.
Title: Euclid: Forecast constraints on consistency tests of the
ΛCDM model
Authors: Nesseris, S.; Sapone, D.; Martinelli, M.; Camarena, D.; Marra,
V.; Sakr, Z.; Garcia-Bellido, J.; Martins, C. J. A. P.; Clarkson, C.;
Da Silva, A.; Fleury, P.; Lombriser, L.; Mimoso, J. P.; Casas, S.;
Pettorino, V.; Tutusaus, I.; Amara, A.; Auricchio, N.; Bodendorf, C.;
Bonino, D.; Branchini, E.; Brescia, M.; Capobianco, V.; Carbone, C.;
Carretero, J.; Castellano, M.; Cavuoti, S.; Cimatti, A.; Cledassou,
R.; Congedo, G.; Conversi, L.; Copin, Y.; Corcione, L.; Courbin, F.;
Cropper, M.; Degaudenzi, H.; Douspis, M.; Dubath, F.; Duncan, C. A. J.;
Dupac, X.; Dusini, S.; Ealet, A.; Farrens, S.; Fosalba, P.; Frailis,
M.; Franceschi, E.; Fumana, M.; Garilli, B.; Gillis, B.; Giocoli,
C.; Grazian, A.; Grupp, F.; Haugan, S. V. H.; Holmes, W.; Hormuth,
F.; Jahnke, K.; Kermiche, S.; Kiessling, A.; Kitching, T.; Kümmel,
M.; Kunz, M.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro,
I.; Mansutti, O.; Marggraf, O.; Markovic, K.; Marulli, F.; Massey,
R.; Meneghetti, M.; Merlin, E.; Meylan, G.; Moresco, M.; Moscardini,
L.; Munari, E.; Niemi, S. M.; Padilla, C.; Paltani, S.; Pasian, F.;
Pedersen, K.; Percival, W. J.; Poncet, M.; Popa, L.; Racca, G. D.;
Raison, F.; Rhodes, J.; Roncarelli, M.; Saglia, R.; Sartoris, B.;
Schneider, P.; Secroun, A.; Seidel, G.; Serrano, S.; Sirignano, C.;
Sirri, G.; Stanco, L.; Starck, J. -L.; Tallada-Crespí, P.; Taylor,
A. N.; Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.; Valentijn, E. A.;
Valenziano, L.; Wang, Y.; Welikala, N.; Zamorani, G.; Zoubian, J.;
Andreon, S.; Baldi, M.; Camera, S.; Medinaceli, E.; Mei, S.; Renzi, A.
Bibcode: 2022A&A...660A..67N
Altcode: 2021arXiv211011421N
Context. The standard cosmological model is based on the fundamental
assumptions of a spatially homogeneous and isotropic universe on
large scales. An observational detection of a violation of these
assumptions at any redshift would immediately indicate the presence of
new physics.
Aims: We quantify the ability of the Euclid mission,
together with contemporary surveys, to improve the current sensitivity
of null tests of the canonical cosmological constant Λ and the cold
dark matter (ΛCDM) model in the redshift range 0 < z < 1.8.
Methods: We considered both currently available data and simulated
Euclid and external data products based on a ΛCDM fiducial model,
an evolving dark energy model assuming the Chevallier-Polarski-Linder
parameterization or an inhomogeneous Lemaître-Tolman-Bondi model with a
cosmological constant Λ, and carried out two separate but complementary
analyses: a machine learning reconstruction of the null tests based on
genetic algorithms, and a theory-agnostic parametric approach based on
Taylor expansion and binning of the data, in order to avoid assumptions
about any particular model.
Results: We find that in combination
with external probes, Euclid can improve current constraints on null
tests of the ΛCDM by approximately a factor of three when using the
machine learning approach and by a further factor of two in the case of
the parametric approach. However, we also find that in certain cases,
the parametric approach may be biased against or missing some features
of models far from ΛCDM.
Conclusions: Our analysis highlights
the importance of synergies between Euclid and other surveys. These
synergies are crucial for providing tighter constraints over an extended
redshift range for a plethora of different consistency tests of some
of the main assumptions of the current cosmological paradigm. This
paper is published on behalf of the Euclid Consortium.
Title: Euclid: Covariance of weak lensing pseudo-Cℓ
estimates. Calculation, comparison to simulations, and dependence
on survey geometry
Authors: Upham, R. E.; Brown, M. L.; Whittaker, L.; Amara, A.;
Auricchio, N.; Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann,
J.; Capobianco, V.; Carbone, C.; Carretero, J.; Castellano, M.;
Cavuoti, S.; Cimatti, A.; Cledassou, R.; Congedo, G.; Conversi,
L.; Copin, Y.; Corcione, L.; Cropper, M.; Da Silva, A.; Degaudenzi,
H.; Douspis, M.; Dubath, F.; Duncan, C. A. J.; Dupac, X.; Dusini,
S.; Ealet, A.; Farrens, S.; Ferriol, S.; Fosalba, P.; Frailis, M.;
Franceschi, E.; Fumana, M.; Garilli, B.; Gillis, B.; Giocoli, C.;
Grupp, F.; Haugan, S. V. H.; Hoekstra, H.; Holmes, W.; Hormuth, F.;
Hornstrup, A.; Jahnke, K.; Kermiche, S.; Kiessling, A.; Kilbinger,
M.; Kitching, T.; Kümmel, M.; Kunz, M.; Kurki-Suonio, H.; Ligori,
S.; Lilje, P. B.; Lloro, I.; Marggraf, O.; Markovic, K.; Marulli,
F.; Meneghetti, M.; Meylan, G.; Moresco, M.; Moscardini, L.; Munari,
E.; Niemi, S. M.; Padilla, C.; Paltani, S.; Pasian, F.; Pedersen,
K.; Pettorino, V.; Pires, S.; Poncet, M.; Popa, L.; Raison, F.;
Rhodes, J.; Rossetti, E.; Saglia, R.; Sartoris, B.; Schneider,
P.; Secroun, A.; Seidel, G.; Sirignano, C.; Sirri, G.; Stanco, L.;
Starck, J. -L.; Tallada-Crespí, P.; Tavagnacco, D.; Taylor, A. N.;
Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.; Valenziano, L.; Wang,
Y.; Zamorani, G.; Zoubian, J.; Andreon, S.; Baldi, M.; Camera, S.;
Cardone, V. F.; Fabbian, G.; Polenta, G.; Renzi, A.; Joachimi, B.;
Hall, A.; Loureiro, A.; Sellentin, E.
Bibcode: 2022A&A...660A.114U
Altcode: 2021arXiv211207341U
An accurate covariance matrix is essential for obtaining reliable
cosmological results when using a Gaussian likelihood. In this
paper we study the covariance of pseudo-Cℓ estimates of
tomographic cosmic shear power spectra. Using two existing publicly
available codes in combination, we calculate the full covariance matrix,
including mode-coupling contributions arising from both partial sky
coverage and non-linear structure growth. For three different sky
masks, we compare the theoretical covariance matrix to that estimated
from publicly available N-body weak lensing simulations, finding
good agreement. We find that as a more extreme sky cut is applied,
a corresponding increase in both Gaussian off-diagonal covariance
and non-Gaussian super-sample covariance is observed in both theory
and simulations, in accordance with expectations. Studying the
different contributions to the covariance in detail, we find that
the Gaussian covariance dominates along the main diagonal and the
closest off-diagonals, but farther away from the main diagonal the
super-sample covariance is dominant. Forming mock constraints in
parameters that describe matter clustering and dark energy, we find
that neglecting non-Gaussian contributions to the covariance can lead
to underestimating the true size of confidence regions by up to 70 per
cent. The dominant non-Gaussian covariance component is the super-sample
covariance, but neglecting the smaller connected non-Gaussian covariance
can still lead to the underestimation of uncertainties by 10-20 per
cent. A real cosmological analysis will require marginalisation over
many nuisance parameters, which will decrease the relative importance
of all cosmological contributions to the covariance, so these values
should be taken as upper limits on the importance of each component. This paper is published on behalf of the Euclid Consortium.
Title: Euclid: Searching for pair-instability supernovae with the
Deep Survey
Authors: Moriya, T. J.; Inserra, C.; Tanaka, M.; Cappellaro, E.; Della
Valle, M.; Hook, I.; Kotak, R.; Longo, G.; Mannucci, F.; Mattila,
S.; Tao, C.; Altieri, B.; Amara, A.; Auricchio, N.; Bonino, D.;
Branchini, E.; Brescia, M.; Brinchmann, J.; Camera, S.; Capobianco,
V.; Carbone, C.; Carretero, J.; Castellano, M.; Cavuoti, S.; Cimatti,
A.; Cledassou, R.; Congedo, G.; Conselice, C. J.; Conversi, L.; Copin,
Y.; Corcione, L.; Courbin, F.; Cropper, M.; Da Silva, A.; Degaudenzi,
H.; Douspis, M.; Dubath, F.; Duncan, C. A. J.; Dupac, X.; Dusini,
S.; Ealet, A.; Farrens, S.; Ferriol, S.; Frailis, M.; Franceschi,
E.; Fumana, M.; Garilli, B.; Gillard, W.; Gillis, B.; Giocoli, C.;
Grazian, A.; Grupp, F.; Haugan, S. V. H.; Holmes, W.; Hormuth, F.;
Hornstrup, A.; Jahnke, K.; Kermiche, S.; Kiessling, A.; Kilbinger, M.;
Kitching, T.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro, I.;
Maiorano, E.; Mansutti, O.; Marggraf, O.; Markovic, K.; Marulli, F.;
Massey, R.; McCracken, H. J.; Melchior, M.; Meneghetti, M.; Meylan,
G.; Moresco, M.; Moscardini, L.; Munari, E.; Niemi, S. M.; Padilla,
C.; Paltani, S.; Pasian, F.; Pedersen, K.; Pettorino, V.; Poncet, M.;
Popa, L.; Raison, F.; Rhodes, J.; Riccio, G.; Rossetti, E.; Saglia,
R.; Sartoris, B.; Schneider, P.; Secroun, A.; Seidel, G.; Sirignano,
C.; Sirri, G.; Stanco, L.; Tallada-Crespí, P.; Taylor, A. N.; Tereno,
I.; Toledo-Moreo, R.; Torradeflot, F.; Wang, Y.; Zamorani, G.; Zoubian,
J.; Andreon, S.; Scottez, V.; Morris, P. W.
Bibcode: 2022arXiv220408727M
Altcode:
Pair-instability supernovae are theorized supernovae that have not
yet been observationally confirmed. They are predicted to exist in
low-metallicity environments. Because overall metallicity becomes lower
at higher redshifts, deep near-infrared transient surveys probing
high-redshift supernovae are suitable to discover pair-instability
supernovae. The Euclid satellite, which is planned to be launched in
2023, has a near-infrared wide-field instrument that is suitable for
a high-redshift supernova survey. The Euclid Deep Survey is planned
to make regular observations of three Euclid Deep Fields (40 deg2
in total) spanning the Euclid's 6 year primary mission period. While
the observations of the Euclid Deep Fields are not frequent, we show
that the predicted long duration of pair-instability supernovae would
allow us to search for high-redshift pair-instability supernovae with
the Euclid Deep Survey. Based on the current observational plan of the
Euclid mission, we conduct survey simulations in order to estimate the
expected numbers of pair-instability supernova discoveries. We find
that up to several hundred pair-instability supernovae at z < ~
3.5 can be discovered within the Euclid Deep Survey. We also show that
pair-instability supernova candidates can be efficiently identified by
their duration and color that can be determined with the current Euclid
Deep Survey plan. We conclude that the Euclid mission can lead to the
first confirmation of pair-instability supernovae if their event rates
are as high as those predicted by recent theoretical studies. We also
update the expected numbers of superluminous supernova discoveries in
the Euclid Deep Survey based on the latest observational plan.
Title: The Solar ALMA Science Archive (SALSA). First release, SALAT,
and FITS header standard
Authors: Henriques, Vasco M. J.; Jafarzadeh, Shahin; Guevara Gómez,
Juan Camilo; Eklund, Henrik; Wedemeyer, Sven; Szydlarski, Mikołaj;
Haugan, Stein Vidar H.; Mohan, Atul
Bibcode: 2022A&A...659A..31H
Altcode: 2021arXiv210902374H
In December 2016, the Atacama Large Millimeter/submillimeter Array
(ALMA) carried out the first regular observations of the Sun. These
early observations and the reduction of the respective data posed a
challenge due to the novelty and complexity of observing the Sun with
ALMA. The difficulties with producing science-ready, time-resolved
imaging products in a format familiar to and usable by solar physicists
based on the measurement sets delivered by ALMA had limited the
availability of such data to this point. With the development of the
Solar ALMA Pipeline, it has now become possible to routinely reduce
such data sets. As a result, a growing number of science-ready solar
ALMA data sets are now offered in the form of the Solar ALMA Science
Archive (SALSA). So far, SALSA contains primarily time series of
single-pointing interferometric images at cadences of one or two
seconds, accompanied by the respective single-dish full-disc solar
images. The data arrays are provided in FITS format. We also present
the first version of a standardised header format that accommodates
future expansions and fits within the scope of other standards
including the ALMA Science Archive itself and SOLARNET. The headers
include information designed to aid the reproduction of the imaging
products from the raw data. Links to co-observations, if available,
with a focus on those of the Interface Region Imaging Spectrograph,
are also provided. SALSA is accompanied by the Solar ALMA Library of
Auxiliary Tools (SALAT), which contains Interactive Data Language and
Python routines for convenient loading and a quick-look analysis of
SALSA data. Movies associated to Figs. 3 and 4 are available at https://www.aanda.org
Title: Euclid: Forecasts from redshift-space distortions and the
Alcock-Paczynski test with cosmic voids
Authors: Hamaus, N.; Aubert, M.; Pisani, A.; Contarini, S.; Verza,
G.; Cousinou, M. -C.; Escoffier, S.; Hawken, A.; Lavaux, G.; Pollina,
G.; Wandelt, B. D.; Weller, J.; Bonici, M.; Carbone, C.; Guzzo, L.;
Kovacs, A.; Marulli, F.; Massara, E.; Moscardini, L.; Ntelis, P.;
Percival, W. J.; Radinović, S.; Sahlén, M.; Sakr, Z.; Sánchez,
A. G.; Winther, H. A.; Auricchio, N.; Awan, S.; Bender, R.; Bodendorf,
C.; Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann, J.; Capobianco,
V.; Carretero, J.; Castander, F. J.; Castellano, M.; Cavuoti, S.;
Cimatti, A.; Cledassou, R.; Congedo, G.; Conversi, L.; Copin, Y.;
Corcione, L.; Cropper, M.; Da Silva, A.; Degaudenzi, H.; Douspis,
M.; Dubath, F.; Duncan, C. A. J.; Dupac, X.; Dusini, S.; Ealet, A.;
Ferriol, S.; Fosalba, P.; Frailis, M.; Franceschi, E.; Franzetti, P.;
Fumana, M.; Garilli, B.; Gillis, B.; Giocoli, C.; Grazian, A.; Grupp,
F.; Haugan, S. V. H.; Holmes, W.; Hormuth, F.; Jahnke, K.; Kermiche,
S.; Kiessling, A.; Kilbinger, M.; Kitching, T.; Kümmel, M.; Kunz, M.;
Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro, I.; Maiorano, E.;
Marggraf, O.; Markovic, K.; Massey, R.; Maurogordato, S.; Melchior,
M.; Meneghetti, M.; Meylan, G.; Moresco, M.; Munari, E.; Niemi, S. M.;
Padilla, C.; Paltani, S.; Pasian, F.; Pedersen, K.; Pettorino, V.;
Pires, S.; Poncet, M.; Popa, L.; Pozzetti, L.; Rebolo, R.; Rhodes,
J.; Rix, H.; Roncarelli, M.; Rossetti, E.; Saglia, R.; Schneider,
P.; Secroun, A.; Seidel, G.; Serrano, S.; Sirignano, C.; Sirri, G.;
Starck, J. -L.; Tallada-Crespí, P.; Tavagnacco, D.; Taylor, A. N.;
Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.; Valentijn, E. A.;
Valenziano, L.; Wang, Y.; Welikala, N.; Zamorani, G.; Zoubian, J.;
Andreon, S.; Baldi, M.; Camera, S.; Mei, S.; Neissner, C.; Romelli, E.
Bibcode: 2022A&A...658A..20H
Altcode: 2021arXiv210810347H
Euclid is poised to survey galaxies across a cosmological volume of
unprecedented size, providing observations of more than a billion
objects distributed over a third of the full sky. Approximately 20
million of these galaxies will have their spectroscopy available,
allowing us to map the three-dimensional large-scale structure of the
Universe in great detail. This paper investigates prospects for the
detection of cosmic voids therein and the unique benefit they provide
for cosmological studies. In particular, we study the imprints of
dynamic (redshift-space) and geometric (Alcock-Paczynski) distortions
of average void shapes and their constraining power on the growth of
structure and cosmological distance ratios. To this end, we made use
of the Flagship mock catalog, a state-of-the-art simulation of the
data expected to be observed with Euclid. We arranged the data into
four adjacent redshift bins, each of which contains about 11 000 voids
and we estimated the stacked void-galaxy cross-correlation function
in every bin. Fitting a linear-theory model to the data, we obtained
constraints on f/b and DMH, where f is the linear growth
rate of density fluctuations, b the galaxy bias, DM the
comoving angular diameter distance, and H the Hubble rate. In addition,
we marginalized over two nuisance parameters included in our model
to account for unknown systematic effects in the analysis. With this
approach, Euclid will be able to reach a relative precision of about
4% on measurements of f/b and 0.5% on DMH in each redshift
bin. Better modeling or calibration of the nuisance parameters may
further increase this precision to 1% and 0.4%, respectively. Our
results show that the exploitation of cosmic voids in Euclid will
provide competitive constraints on cosmology even as a stand-alone
probe. For example, the equation-of-state parameter, w, for dark energy
will be measured with a precision of about 10%, consistent with previous
more approximate forecasts. This paper is published on behalf of
the Euclid Consortium.
Title: Euclid preparation. XVII. Cosmic Dawn Survey: Spitzer Space
Telescope observations of the Euclid deep fields and calibration
fields
Authors: Euclid Collaboration; Moneti, A.; McCracken, H. J.;
Shuntov, M.; Kauffmann, O. B.; Capak, P.; Davidzon, I.; Ilbert, O.;
Scarlata, C.; Toft, S.; Weaver, J.; Chary, R.; Cuby, J.; Faisst,
A. L.; Masters, D. C.; McPartland, C.; Mobasher, B.; Sanders, D. B.;
Scaramella, R.; Stern, D.; Szapudi, I.; Teplitz, H.; Zalesky, L.;
Amara, A.; Auricchio, N.; Bodendorf, C.; Bonino, D.; Branchini, E.;
Brau-Nogue, S.; Brescia, M.; Brinchmann, J.; Capobianco, V.; Carbone,
C.; Carretero, J.; Castander, F. J.; Castellano, M.; Cavuoti, S.;
Cimatti, A.; Cledassou, R.; Congedo, G.; Conselice, C. J.; Conversi,
L.; Copin, Y.; Corcione, L.; Costille, A.; Cropper, M.; Da Silva,
A.; Degaudenzi, H.; Douspis, M.; Dubath, F.; Duncan, C. A. J.; Dupac,
X.; Dusini, S.; Farrens, S.; Ferriol, S.; Fosalba, P.; Frailis, M.;
Franceschi, E.; Fumana, M.; Garilli, B.; Gillis, B.; Giocoli, C.;
Granett, B. R.; Grazian, A.; Grupp, F.; Haugan, S. V. H.; Hoekstra,
H.; Holmes, W.; Hormuth, F.; Hudelot, P.; Jahnke, K.; Kermiche, S.;
Kiessling, A.; Kilbinger, M.; Kitching, T.; Kohley, R.; Kümmel,
M.; Kunz, M.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro, I.;
Maiorano, E.; Mansutti, O.; Marggraf, O.; Markovic, K.; Marulli, F.;
Massey, R.; Maurogordato, S.; Meneghetti, M.; Merlin, E.; Meylan,
G.; Moresco, M.; Moscardini, L.; Munari, E.; Niemi, S. M.; Padilla,
C.; Paltani, S.; Pasian, F.; Pedersen, K.; Pires, S.; Poncet, M.;
Popa, L.; Pozzetti, L.; Raison, F.; Rebolo, R.; Rhodes, J.; Rix, H.;
Roncarelli, M.; Rossetti, E.; Saglia, R.; Schneider, P.; Secroun,
A.; Seidel, G.; Serrano, S.; Sirignano, C.; Sirri, G.; Stanco, L.;
Tallada-Crespí, P.; Taylor, A. N.; Tereno, I.; Toledo-Moreo, R.;
Torradeflot, F.; Wang, Y.; Welikala, N.; Weller, J.; Zamorani, G.;
Zoubian, J.; Andreon, S.; Bardelli, S.; Camera, S.; Graciá-Carpio,
J.; Medinaceli, E.; Mei, S.; Polenta, G.; Romelli, E.; Sureau, F.;
Tenti, M.; Vassallo, T.; Zacchei, A.; Zucca, E.; Baccigalupi, C.;
Balaguera-Antolínez, A.; Bernardeau, F.; Biviano, A.; Bolzonella,
M.; Bozzo, E.; Burigana, C.; Cabanac, R.; Cappi, A.; Carvalho, C. S.;
Casas, S.; Castignani, G.; Colodro-Conde, C.; Coupon, J.; Courtois,
H. M.; Di Ferdinando, D.; Farina, M.; Finelli, F.; Flose-Reimberg, P.;
Fotopoulou, S.; Galeotta, S.; Ganga, K.; Garcia-Bellido, J.; Gaztanaga,
E.; Gozaliasl, G.; Hook, I.; Joachimi, B.; Kansal, V.; Keihanen, E.;
Kirkpatrick, C. C.; Lindholm, V.; Mainetti, G.; Maino, D.; Maoli, R.;
Martinelli, M.; Martinet, N.; Maturi, M.; Metcalf, R. B.; Morgante,
G.; Morisset, N.; Nucita, A.; Patrizii, L.; Potter, D.; Renzi, A.;
Riccio, G.; Sánchez, A. G.; Sapone, D.; Schirmer, M.; Schultheis,
M.; Scottez, V.; Sefusatti, E.; Teyssier, R.; Tubio, O.; Tutusaus,
I.; Valiviita, J.; Viel, M.; Hildebrandt, H.
Bibcode: 2022A&A...658A.126E
Altcode: 2021arXiv211013928M
We present a new infrared survey covering the three Euclid deep
fields and four other Euclid calibration fields using Spitzer
Space Telescope's Infrared Array Camera (IRAC). We combined these
new observations with all relevant IRAC archival data of these
fields in order to produce the deepest possible mosaics of these
regions. In total, these observations represent nearly 11 % of the
total Spitzer Space Telescope mission time. The resulting mosaics
cover a total of approximately 71.5 deg2 in the 3.6 and
4.5 μm bands, and approximately 21.8 deg2 in the 5.8 and
8 μm bands. They reach at least 24 AB magnitude (measured to 5σ,
in a 2″.5 aperture) in the 3.6 μm band and up to ∼5 mag deeper
in the deepest regions. The astrometry is tied to the Gaia astrometric
reference system, and the typical astrometric uncertainty for sources
with 16 < [3.6]< 19 is ≲0″.15. The photometric calibration is
in excellent agreement with previous WISE measurements. We extracted
source number counts from the 3.6 μm band mosaics, and they are in
excellent agreement with previous measurements. Given that the Spitzer
Space Telescope has now been decommissioned, these mosaics are likely to
be the definitive reduction of these IRAC data. This survey therefore
represents an essential first step in assembling multi-wavelength data
on the Euclid deep fields, which are set to become some of the premier
fields for extragalactic astronomy in the 2020s.
Title: Euclid preparation. XVI. Exploring the ultra-low surface
brightness Universe with Euclid/VIS
Authors: Euclid Collaboration; Borlaff, A. S.; Gómez-Alvarez, P.;
Altieri, B.; Marcum, P. M.; Vavrek, R.; Laureijs, R.; Kohley, R.;
Buitrago, F.; Cuillandre, J. -C.; Duc, P. -A.; Gaspar Venancio, L. M.;
Amara, A.; Andreon, S.; Auricchio, N.; Azzollini, R.; Baccigalupi,
C.; Balaguera-Antolínez, A.; Baldi, M.; Bardelli, S.; Bender, R.;
Biviano, A.; Bodendorf, C.; Bonino, D.; Bozzo, E.; Branchini, E.;
Brescia, M.; Brinchmann, J.; Burigana, C.; Cabanac, R.; Camera, S.;
Candini, G. P.; Capobianco, V.; Cappi, A.; Carbone, C.; Carretero,
J.; Carvalho, C. S.; Casas, S.; Castander, F. J.; Castellano, M.;
Castignani, G.; Cavuoti, S.; Cimatti, A.; Cledassou, R.; Colodro-Conde,
C.; Congedo, G.; Conselice, C. J.; Conversi, L.; Copin, Y.; Corcione,
L.; Coupon, J.; Courtois, H. M.; Cropper, M.; Da Silva, A.; Degaudenzi,
H.; Di Ferdinando, D.; Douspis, M.; Dubath, F.; Duncan, C. A. J.;
Dupac, X.; Dusini, S.; Ealet, A.; Fabricius, M.; Farina, M.; Farrens,
S.; Ferreira, P. G.; Ferriol, S.; Finelli, F.; Flose-Reimberg, P.;
Fosalba, P.; Frailis, M.; Franceschi, E.; Fumana, M.; Galeotta,
S.; Ganga, K.; Garilli, B.; Gillis, B.; Giocoli, C.; Gozaliasl, G.;
Graciá-Carpio, J.; Grazian, A.; Grupp, F.; Haugan, S. V. H.; Holmes,
W.; Hormuth, F.; Jahnke, K.; Keihanen, E.; Kermiche, S.; Kiessling,
A.; Kilbinger, M.; Kirkpatrick, C. C.; Kitching, T.; Knapen, J. H.;
Kubik, B.; Kümmel, M.; Kunz, M.; Kurki-Suonio, H.; Liebing, P.;
Ligori, S.; Lilje, P. B.; Lindholm, V.; Lloro, I.; Mainetti, G.;
Maino, D.; Mansutti, O.; Marggraf, O.; Markovic, K.; Martinelli, M.;
Martinet, N.; Martínez-Delgado, D.; Marulli, F.; Massey, R.; Maturi,
M.; Maurogordato, S.; Medinaceli, E.; Mei, S.; Meneghetti, M.; Merlin,
E.; Metcalf, R. B.; Meylan, G.; Moresco, M.; Morgante, G.; Moscardini,
L.; Munari, E.; Nakajima, R.; Neissner, C.; Niemi, S. M.; Nightingale,
J. W.; Nucita, A.; Padilla, C.; Paltani, S.; Pasian, F.; Patrizii,
L.; Pedersen, K.; Percival, W. J.; Pettorino, V.; Pires, S.; Poncet,
M.; Popa, L.; Potter, D.; Pozzetti, L.; Raison, F.; Rebolo, R.; Renzi,
A.; Rhodes, J.; Riccio, G.; Romelli, E.; Roncarelli, M.; Rosset, C.;
Rossetti, E.; Saglia, R.; Sánchez, A. G.; Sapone, D.; Sauvage, M.;
Schneider, P.; Scottez, V.; Secroun, A.; Seidel, G.; Serrano, S.;
Sirignano, C.; Sirri, G.; Skottfelt, J.; Stanco, L.; Starck, J. L.;
Sureau, F.; Tallada-Crespí, P.; Taylor, A. N.; Tenti, M.; Tereno,
I.; Teyssier, R.; Toledo-Moreo, R.; Torradeflot, F.; Tutusaus, I.;
Valentijn, E. A.; Valenziano, L.; Valiviita, J.; Vassallo, T.; Viel,
M.; Wang, Y.; Weller, J.; Whittaker, L.; Zacchei, A.; Zamorani, G.;
Zucca, E.
Bibcode: 2022A&A...657A..92E
Altcode: 2021arXiv210810321B
Context. While Euclid is an ESA mission specifically designed to
investigate the nature of dark energy and dark matter, the planned
unprecedented combination of survey area (∼15 000 deg2),
spatial resolution, low sky-background, and depth also make Euclid an
excellent space observatory for the study of the low surface brightness
Universe. Scientific exploitation of the extended low surface brightness
structures requires dedicated calibration procedures that are yet to
be tested.
Aims: We investigate the capabilities of Euclid to
detect extended low surface brightness structure by identifying and
quantifying sky-background sources and stray-light contamination. We
test the feasibility of generating sky flat-fields to reduce large-scale
residual gradients in order to reveal the extended emission of galaxies
observed in the Euclid survey.
Methods: We simulated a realistic
set of Euclid/VIS observations, taking into account both instrumental
and astronomical sources of contamination, including cosmic rays,
stray-light, zodiacal light, interstellar medium, and the cosmic
infrared background, while simulating the effects of background
sources in the field of view.
Results: We demonstrate that
a combination of calibration lamps, sky flats, and self-calibration
would enable recovery of emission at a limiting surface brightness
magnitude of μlim = 29.5−0.27+0.08
mag arcsec−2 (3σ, 10 × 10 arcsec2) in
the Wide Survey, and it would reach regions deeper by 2 mag in
the Deep Surveys. Conclusions.Euclid/VIS has the potential to be
an excellent low surface brightness observatory. Covering the gap
between pixel-to-pixel calibration lamp flats and self-calibration
observations for large scales, the application of sky flat-fielding
will enhance the sensitivity of the VIS detector at scales larger
than 1″, up to the size of the field of view, enabling Euclid to
detect extended surface brightness structures below μlim
= 31 mag arcsec−2 and beyond.
Title: Euclid preparation. XIII. Forecasts for galaxy morphology
with the Euclid Survey using deep generative models
Authors: Euclid Collaboration; Bretonnière, H.; Huertas-Company,
M.; Boucaud, A.; Lanusse, F.; Jullo, E.; Merlin, E.; Tuccillo, D.;
Castellano, M.; Brinchmann, J.; Conselice, C. J.; Dole, H.; Cabanac,
R.; Courtois, H. M.; Castander, F. J.; Duc, P. A.; Fosalba, P.; Guinet,
D.; Kruk, S.; Kuchner, U.; Serrano, S.; Soubrie, E.; Tramacere,
A.; Wang, L.; Amara, A.; Auricchio, N.; Bender, R.; Bodendorf, C.;
Bonino, D.; Branchini, E.; Brau-Nogue, S.; Brescia, M.; Capobianco,
V.; Carbone, C.; Carretero, J.; Cavuoti, S.; Cimatti, A.; Cledassou,
R.; Congedo, G.; Conversi, L.; Copin, Y.; Corcione, L.; Costille, A.;
Cropper, M.; Da Silva, A.; Degaudenzi, H.; Douspis, M.; Dubath, F.;
Duncan, C. A. J.; Dupac, X.; Dusini, S.; Farrens, S.; Ferriol, S.;
Frailis, M.; Franceschi, E.; Fumana, M.; Garilli, B.; Gillard, W.;
Gillis, B.; Giocoli, C.; Grazian, A.; Grupp, F.; Haugan, S. V. H.;
Holmes, W.; Hormuth, F.; Hudelot, P.; Jahnke, K.; Kermiche, S.;
Kiessling, A.; Kilbinger, M.; Kitching, T.; Kohley, R.; Kümmel,
M.; Kunz, M.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro, I.;
Maiorano, E.; Mansutti, O.; Marggraf, O.; Markovic, K.; Marulli, F.;
Massey, R.; Maurogordato, S.; Melchior, M.; Meneghetti, M.; Meylan,
G.; Moresco, M.; Morin, B.; Moscardini, L.; Munari, E.; Nakajima,
R.; Niemi, S. M.; Padilla, C.; Paltani, S.; Pasian, F.; Pedersen, K.;
Pettorino, V.; Pires, S.; Poncet, M.; Popa, L.; Pozzetti, L.; Raison,
F.; Rebolo, R.; Rhodes, J.; Roncarelli, M.; Rossetti, E.; Saglia,
R.; Schneider, P.; Secroun, A.; Seidel, G.; Sirignano, C.; Sirri, G.;
Stanco, L.; Starck, J. -L.; Tallada-Crespí, P.; Taylor, A. N.; Tereno,
I.; Toledo-Moreo, R.; Torradeflot, F.; Valentijn, E. A.; Valenziano,
L.; Wang, Y.; Welikala, N.; Weller, J.; Zamorani, G.; Zoubian, J.;
Baldi, M.; Bardelli, S.; Camera, S.; Farinelli, R.; Medinaceli, E.;
Mei, S.; Polenta, G.; Romelli, E.; Tenti, M.; Vassallo, T.; Zacchei,
A.; Zucca, E.; Baccigalupi, C.; Balaguera-Antolínez, A.; Biviano,
A.; Borgani, S.; Bozzo, E.; Burigana, C.; Cappi, A.; Carvalho, C. S.;
Casas, S.; Castignani, G.; Colodro-Conde, C.; Coupon, J.; de la Torre,
S.; Fabricius, M.; Farina, M.; Ferreira, P. G.; Flose-Reimberg, P.;
Fotopoulou, S.; Galeotta, S.; Ganga, K.; Garcia-Bellido, J.; Gaztanaga,
E.; Gozaliasl, G.; Hook, I. M.; Joachimi, B.; Kansal, V.; Kashlinsky,
A.; Keihanen, E.; Kirkpatrick, C. C.; Lindholm, V.; Mainetti, G.;
Maino, D.; Maoli, R.; Martinelli, M.; Martinet, N.; McCracken, H. J.;
Metcalf, R. B.; Morgante, G.; Morisset, N.; Nightingale, J.; Nucita,
A.; Patrizii, L.; Potter, D.; Renzi, A.; Riccio, G.; Sánchez, A. G.;
Sapone, D.; Schirmer, M.; Schultheis, M.; Scottez, V.; Sefusatti,
E.; Teyssier, R.; Tutusaus, I.; Valiviita, J.; Viel, M.; Whittaker,
L.; Knapen, J. H.
Bibcode: 2022A&A...657A..90E
Altcode: 2021arXiv210512149B; 2021arXiv210512149E
We present a machine learning framework to simulate realistic galaxies
for the Euclid Survey, producing more complex and realistic galaxies
than the analytical simulations currently used in Euclid. The proposed
method combines a control on galaxy shape parameters offered by analytic
models with realistic surface brightness distributions learned from
real Hubble Space Telescope observations by deep generative models. We
simulate a galaxy field of 0.4 deg2 as it will be seen by
the Euclid visible imager VIS, and we show that galaxy structural
parameters are recovered to an accuracy similar to that for pure
analytic Sérsic profiles. Based on these simulations, we estimate
that the Euclid Wide Survey (EWS) will be able to resolve the internal
morphological structure of galaxies down to a surface brightness of
22.5 mag arcsec−2, and the Euclid Deep Survey (EDS) down
to 24.9 mag arcsec−2. This corresponds to approximately
250 million galaxies at the end of the mission and a 50% complete
sample for stellar masses above 1010.6 M⊙
(resp. 109.6 M⊙) at a redshift z ∼ 0.5 for the
EWS (resp. EDS). The approach presented in this work can contribute to
improving the preparation of future high-precision cosmological imaging
surveys by allowing simulations to incorporate more realistic galaxies.
Title: Euclid preparation. XV. Forecasting cosmological constraints
for the Euclid and CMB joint analysis
Authors: Euclid Collaboration; Ilić, S.; Aghanim, N.; Baccigalupi,
C.; Bermejo-Climent, J. R.; Fabbian, G.; Legrand, L.; Paoletti,
D.; Ballardini, M.; Archidiacono, M.; Douspis, M.; Finelli, F.;
Ganga, K.; Hernández-Monteagudo, C.; Lattanzi, M.; Marinucci, D.;
Migliaccio, M.; Carbone, C.; Casas, S.; Martinelli, M.; Tutusaus,
I.; Natoli, P.; Ntelis, P.; Pagano, L.; Wenzl, L.; Gruppuso, A.;
Kitching, T.; Langer, M.; Mauri, N.; Patrizii, L.; Renzi, A.; Sirri,
G.; Stanco, L.; Tenti, M.; Vielzeuf, P.; Lacasa, F.; Polenta, G.;
Yankelevich, V.; Blanchard, A.; Sakr, Z.; Pourtsidou, A.; Camera, S.;
Cardone, V. F.; Kilbinger, M.; Kunz, M.; Markovic, K.; Pettorino, V.;
Sánchez, A. G.; Sapone, D.; Amara, A.; Auricchio, N.; Bender, R.;
Bodendorf, C.; Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann,
J.; Capobianco, V.; Carretero, J.; Castander, F. J.; Castellano,
M.; Cavuoti, S.; Cimatti, A.; Cledassou, R.; Congedo, G.; Conselice,
C. J.; Conversi, L.; Copin, Y.; Corcione, L.; Costille, A.; Cropper,
M.; Da Silva, A.; Degaudenzi, H.; Dubath, F.; Duncan, C. A. J.; Dupac,
X.; Dusini, S.; Ealet, A.; Farrens, S.; Fosalba, P.; Frailis, M.;
Franceschi, E.; Franzetti, P.; Fumana, M.; Garilli, B.; Gillard, W.;
Gillis, B.; Giocoli, C.; Grazian, A.; Grupp, F.; Guzzo, L.; Haugan,
S. V. H.; Hoekstra, H.; Holmes, W.; Hormuth, F.; Hudelot, P.; Jahnke,
K.; Kermiche, S.; Kiessling, A.; Kohley, R.; Kubik, B.; Kümmel, M.;
Kurki-Suonio, H.; Laureijs, R.; Ligori, S.; Lilje, P. B.; Lloro, I.;
Mansutti, O.; Marggraf, O.; Marulli, F.; Massey, R.; Maurogordato,
S.; Meneghetti, M.; Merlin, E.; Meylan, G.; Moresco, M.; Morin, B.;
Moscardini, L.; Munari, E.; Niemi, S. M.; Padilla, C.; Paltani, S.;
Pasian, F.; Pedersen, K.; Percival, W.; Pires, S.; Poncet, M.; Popa,
L.; Pozzetti, L.; Raison, F.; Rebolo, R.; Rhodes, J.; Roncarelli, M.;
Rossetti, E.; Saglia, R.; Scaramella, R.; Schneider, P.; Secroun, A.;
Seidel, G.; Serrano, S.; Sirignano, C.; Starck, J. L.; Tallada-Crespí,
P.; Taylor, A. N.; Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.;
Valentijn, E. A.; Valenziano, L.; Verdoes Kleijn, G. A.; Wang, Y.;
Welikala, N.; Weller, J.; Zamorani, G.; Zoubian, J.; Medinaceli, E.;
Mei, S.; Rosset, C.; Sureau, F.; Vassallo, T.; Zacchei, A.; Andreon,
S.; Balaguera-Antolínez, A.; Baldi, M.; Bardelli, S.; Biviano, A.;
Borgani, S.; Bozzo, E.; Burigana, C.; Cabanac, R.; Cappi, A.; Carvalho,
C. S.; Castignani, G.; Colodro-Conde, C.; Coupon, J.; Courtois, H. M.;
Cuby, J.; de la Torre, S.; Di Ferdinando, D.; Dole, H.; Farina, M.;
Ferreira, P. G.; Flose-Reimberg, P.; Galeotta, S.; Gozaliasl, G.;
Graciá-Carpio, J.; Keihanen, E.; Kirkpatrick, C. C.; Lindholm, V.;
Mainetti, G.; Maino, D.; Martinet, N.; Maturi, M.; Metcalf, R. B.;
Morgante, G.; Neissner, C.; Nightingale, J.; Nucita, A. A.; Potter,
D.; Riccio, G.; Romelli, E.; Schirmer, M.; Schultheis, M.; Scottez,
V.; Teyssier, R.; Tramacere, A.; Valiviita, J.; Viel, M.; Whittaker,
L.; Zucca, E.
Bibcode: 2022A&A...657A..91E
Altcode: 2021arXiv210608346E; 2021arXiv210608346I
The combination and cross-correlation of the upcoming Euclid data with
cosmic microwave background (CMB) measurements is a source of great
expectation since it will provide the largest lever arm of epochs,
ranging from recombination to structure formation across the entire
past light cone. In this work, we present forecasts for the joint
analysis of Euclid and CMB data on the cosmological parameters of the
standard cosmological model and some of its extensions. This work
expands and complements the recently published forecasts based on
Euclid-specific probes, namely galaxy clustering, weak lensing, and
their cross-correlation. With some assumptions on the specifications
of current and future CMB experiments, the predicted constraints are
obtained from both a standard Fisher formalism and a posterior-fitting
approach based on actual CMB data. Compared to a Euclid-only analysis,
the addition of CMB data leads to a substantial impact on constraints
for all cosmological parameters of the standard Λ-cold-dark-matter
model, with improvements reaching up to a factor of ten. For the
parameters of extended models, which include a redshift-dependent dark
energy equation of state, non-zero curvature, and a phenomenological
modification of gravity, improvements can be of the order of two to
three, reaching higher than ten in some cases. The results highlight
the crucial importance for cosmological constraints of the combination
and cross-correlation of Euclid probes with CMB data.
Title: KiDS & Euclid: Cosmological implications of a pseudo
angular power spectrum analysis of KiDS-1000 cosmic shear tomography
Authors: Loureiro, A.; Whittaker, L.; Spurio Mancini, A.; Joachimi, B.;
Cuceu, A.; Asgari, M.; Stölzner, B.; Tröster, T.; Wright, A. H.;
Bilicki, M.; Dvornik, A.; Giblin, B.; Heymans, C.; Hildebrandt,
H.; Shan, H.; Amara, A.; Auricchio, N.; Bodendorf, C.; Bonino, D.;
Branchini, E.; Brescia, M.; Capobianco, V.; Carbone, C.; Carretero,
J.; Castellano, M.; Cavuoti, S.; Cimatti, A.; Cledassou, R.; Congedo,
G.; Conversi, L.; Copin, Y.; Corcione, L.; Cropper, M.; Da Silva,
A.; Douspis, M.; Dubath, F.; Duncan, C. A. J.; Dupac, X.; Dusini, S.;
Farrens, S.; Ferriol, S.; Fosalba, P.; Frailis, M.; Franceschi, E.;
Fumana, M.; Garilli, B.; Gillis, B.; Giocoli, C.; Grazian, A.; Grupp,
F.; Haugan, S. V. H.; Holmes, W.; Hormuth, F.; Jahnke, K.; Kermiche,
S.; Kiessling, A.; Kilbinger, M.; Kitching, T.; Kümmel, M.; Kuijken,
K.; Kunz, M.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro,
I.; Mansutti, O.; Marggraf, O.; Markovic, K.; Marulli, F.; Massey,
R.; Meneghetti, M.; Meylan, G.; Moresco, M.; Morin, B.; Moscardini,
L.; Munari, E.; Niemi, S. M.; Padilla, C.; Paltani, S.; Pasian, F.;
Pedersen, K.; Pettorino, V.; Pires, S.; Poncet, M.; Popa, L.; Raison,
F.; Rhodes, J.; Rix, H.; Roncarelli, M.; Saglia, R.; Schneider, P.;
Secroun, A.; Serrano, S.; Sirignano, C.; Sirri, G.; Stanco, L.; Starck,
J. L.; Tallada-Crespí, P.; Taylor, A. N.; Tereno, I.; Toledo-Moreo,
R.; Torradeflot, F.; Valentijn, E. A.; Wang, Y.; Welikala, N.; Weller,
J.; Zamorani, G.; Zoubian, J.; Andreon, S.; Baldi, M.; Camera, S.;
Farinelli, R.; Polenta, G.; Tessore, N.
Bibcode: 2021arXiv211006947L
Altcode:
We present a tomographic weak lensing analysis of the Kilo Degree
Survey Data Release 4 (KiDS-1000), using a new pseudo angular power
spectrum estimator (pseudo-$C_{\ell}$) under development for the
ESA Euclid mission. Over 21 million galaxies with shape information
are divided into five tomographic redshift bins, ranging from 0.1
to 1.2 in photometric redshift. We measured pseudo-$C_{\ell}$ using
eight bands in the multipole range $76<\ell<1500$ for auto-
and cross-power spectra between the tomographic bins. A series of
tests were carried out to check for systematic contamination from
a variety of observational sources including stellar number density,
variations in survey depth, and point spread function properties. While
some marginal correlations with these systematic tracers were observed,
there is no evidence of bias in the cosmological inference. B-mode power
spectra are consistent with zero signal, with no significant residual
contamination from E/B-mode leakage. We performed a Bayesian analysis
of the pseudo-$C_{\ell}$ estimates by forward modelling the effects
of the mask. Assuming a spatially flat $\Lambda$CDM cosmology, we
constrained the structure growth parameter $S_8 = \sigma_8(\Omega_{\rm
m}/0.3)^{1/2} = 0.754_{-0.029}^{+0.027}$. When combining cosmic
shear from KiDS-1000 with baryon acoustic oscillation and redshift
space distortion data from recent Sloan Digital Sky Survey (SDSS)
measurements of luminous red galaxies, as well as the Lyman-$\alpha$
forest and its cross-correlation with quasars, we tightened these
constraints to $S_8 = 0.771^{+0.006}_{-0.032}$. These results are
in very good agreement with previous KiDS-1000 and SDSS analyses and
confirm a $\sim 3\sigma$ tension with early-Universe constraints from
cosmic microwave background experiments.
Title: VizieR Online Data Catalog: Euclid preparation. XIV. C3R2
survey DR3 (Stanford+, 2021)
Authors: Stanford, S. A.; Masters, D.; Darvish, B.; Stern, D.; Cohen,
J. G.; Capak, P.; Hernitschek, N.; Davidzon, I.; Rhodes, J.; Sanders,
D. B.; Mobasher, B.; Castander, F. J.; Paltani, S.; Aghanim, N.;
Amara, A.; Auricchio, N.; Balestra, A.; Bender, R.; Bodendorf, C.;
Bonino, D.; Branchini, E.; Brinchmann, J.; Capobianco, V.; Carbone,
C.; Carretero, J.; Casas, R.; Castellano, M.; Cavuoti, S.; Cimatti, A.;
Cledassou, R.; Conselice, C. J.; Corcione, L.; Costille, A.; Cropper,
M.; Degaudenzi, H.; Douspis, M.; Dubath, F.; Dusini, S.; Fosalba,
P.; Frailis, M.; Franceschi, E.; Franzetti, P.; Fumana, M.; Garilli,
B.; Giocoli, C.; Grupp, F.; Haugan, S. V. H.; Hoekstra, H.; Holmes,
W.; Hormuth, F.; Hudelot, P.; Jahnke, K.; Kiessling, A.; Kilbinger,
M.; Kitching, T.; Kubik, B.; Kummel, M.; Kunz, M.; Kurki-Suonio,
H.; Laureijs, R.; Ligori, S.; Lilje, P. B.; Lloro, I.; Maiorano, E.;
Marggraf, O.; Markovic, K.; Massey, R.; Meneghetti, M.; Meylan, G.;
Moscardini, L.; Niemi, S. M.; Padilla, C.; Pasian, F.; Pedersen,
K.; Pettorino, V.; Pires, S.; Poncet, M.; Popa, L.; Pozzetti, L.;
Raison, F.; Roncarelli, M.; Rossetti, E.; Saglia, R.; Scaramella, R.;
Schneider, P.; Secroun, A.; Seidel, G.; Serrano, S.; Sirignano, C.;
Sirri, G.; Taylor, A. N.; Teplitz, H. I.; Tereno, I.; Toledo-Moreo,
R.; Valentijn, E. A.; Valenziano, L.; Verdoes Kleijn, G. A.; Wang,
Y.; Zamorani, G.; Zoubian, J.; Brescia, M.; Congedo, G.; Conversi, L.;
Copin, Y.; Kermiche, S.; Kohley, R.; Medinaceli, E.; Mei, S.; Moresco,
M.; Morin, B.; Munari, E.; Polenta, G.; Sureau, F.; Tallada Crespi,
P.; Vassallo, T.; Zacchei, A.; Andreon, S.; Aussel, H.; Baccigalupi,
C.; Balaguera-Antolinez, A.; Baldi, M.; Bardelli, S.; Biviano, A.;
Borsato, E.; Bozzo, E.; Burigana, C.; Cabanac, R.; Camera, S.; Cappi,
A.; Carvalho, C. S.; Casas, S.; Castignani, G.; Colodro-Conde, C.;
Coupon, J.; Courtois, H. M.; Cuby, J. -G.; da Silva, A.; de la Torre,
S.; di Ferdinando, D.; Duncan, C. A. J.; Dupac, X.; Fabricius, M.;
Farina, M.; Farrens, S.; Ferreira, P. G.; Finelli, F.; Flose-Reimberg,
P.; Fotopoulou, S.; Galeotta, S.; Ganga, K.; Gillard, W.; Gozaliasl,
G.; Gracia-Carpio, J.; Keihanen, E.; Kirkpatrick, C. C.; Lindholm,
V.; Mainetti, G.; Maino, D.; Martinet, N.; Marulli, F.; Maturi,
M.; Maurogordato, S.; Metcalf, R. B.; Nakajima, R.; Neissner, C.;
Nightingale, J. W.; Nucita, A. A.; Patrizii, L.; Potter, D.; Renzi,
A.; Riccio, G.; Romelli, E.; Sanchez, A. G.; Sapone, D.; Schirmer,
M.; Schultheis, M.; Scottez, V.; Stanco, L.; Tenti, M.; Teyssier,
R.; Torradeflot, F.; Valiviita, J.; Viel, M.; Whittaker, L.; Zucca, E.
Bibcode: 2021yCat..22560009S
Altcode:
The observations were carried out at the Keck Observatory located on
Maunakea in Hawaii. Both of the two 10m telescopes were used, as the Low
Resolution Imaging Spectrometer (LRIS) and Multi-Object Spectrometer
For Infra-Red Exploration (MOSFIRE) are located on KeckI and the DEep
Imaging Multi-Object Spectrograph (DEIMOS) on KeckII. The 19 observing
nights span 2017 Dec 11 to 2020 Oct 19. Observations for DR3
were carried out essentially in the same manner as described in M17
(Masters+ 2017, J/ApJ/841/111) and M19 (Masters+ 2019, J/ApJ/877/81)
for the previous data releases. (2 data files).
Title: Euclid: Constraining dark energy coupled to electromagnetism
using astrophysical and laboratory data
Authors: Martinelli, M.; Martins, C. J. A. P.; Nesseris, S.; Tutusaus,
I.; Blanchard, A.; Camera, S.; Carbone, C.; Casas, S.; Pettorino,
V.; Sakr, Z.; Yankelevich, V.; Sapone, D.; Amara, A.; Auricchio, N.;
Bodendorf, C.; Bonino, D.; Branchini, E.; Capobianco, V.; Carretero,
J.; Castellano, M.; Cavuoti, S.; Cimatti, A.; Cledassou, R.; Corcione,
L.; Costille, A.; Degaudenzi, H.; Douspis, M.; Dubath, F.; Dusini,
S.; Ealet, A.; Ferriol, S.; Frailis, M.; Franceschi, E.; Garilli,
B.; Giocoli, C.; Grazian, A.; Grupp, F.; Haugan, S. V. H.; Holmes,
W.; Hormuth, F.; Jahnke, K.; Kiessling, A.; Kümmel, M.; Kunz, M.;
Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro, I.; Mansutti, O.;
Marggraf, O.; Markovic, K.; Massey, R.; Meneghetti, M.; Meylan, G.;
Moscardini, L.; Niemi, S. M.; Padilla, C.; Paltani, S.; Pasian, F.;
Pedersen, K.; Pires, S.; Poncet, M.; Popa, L.; Raison, F.; Rebolo,
R.; Rhodes, J.; Roncarelli, M.; Rossetti, E.; Saglia, R.; Secroun,
A.; Seidel, G.; Serrano, S.; Sirignano, C.; Sirri, G.; Starck,
J. -L.; Tavagnacco, D.; Taylor, A. N.; Tereno, I.; Toledo-Moreo,
R.; Valenziano, L.; Wang, Y.; Zamorani, G.; Zoubian, J.; Baldi,
M.; Brescia, M.; Congedo, G.; Conversi, L.; Copin, Y.; Fabbian, G.;
Farinelli, R.; Medinaceli, E.; Mei, S.; Polenta, G.; Romelli, E.;
Vassallo, T.
Bibcode: 2021A&A...654A.148M
Altcode: 2021arXiv210509746M
In physically realistic, scalar-field-based dynamical dark energy models
(including, e.g., quintessence), one naturally expects the scalar field
to couple to the rest of the model's degrees of freedom. In particular,
a coupling to the electromagnetic sector leads to a time (redshift)
dependence in the fine-structure constant and a violation of the weak
equivalence principle. Here we extend the previous Euclid forecast
constraints on dark energy models to this enlarged (but physically more
realistic) parameter space, and forecast how well Euclid, together with
high-resolution spectroscopic data and local experiments, can constrain
these models. Our analysis combines simulated Euclid data products
with astrophysical measurements of the fine-structure constant, α,
and local experimental constraints, and it includes both parametric
and non-parametric methods. For the astrophysical measurements of α,
we consider both the currently available data and a simulated dataset
representative of Extremely Large Telescope measurements that are
expected to be available in the 2030s. Our parametric analysis shows
that in the latter case, the inclusion of astrophysical and local data
improves the Euclid dark energy figure of merit by between 8% and
26%, depending on the correct fiducial model, with the improvements
being larger in the null case where the fiducial coupling to the
electromagnetic sector is vanishing. These improvements would be
smaller with the current astrophysical data. Moreover, we illustrate
how a genetic algorithms based reconstruction provides a null test for
the presence of the coupling. Our results highlight the importance
of complementing surveys like Euclid with external data products,
in order to accurately test the wider parameter spaces of physically
motivated paradigms. This paper is published on behalf of the
Euclid Consortium.
Title: Euclid: Estimation of the Impact of Correlated Readout Noise
for Flux Measurements with the Euclid NISP Instrument
Authors: Jiménez Muñoz, A.; Macías-Pérez, J.; Secroun, A.; Gillard,
W.; Kubik, B.; Auricchio, N.; Balestra, A.; Bodendorf, C.; Bonino, D.;
Branchini, E.; Brescia, M.; Brinchmann, J.; Capobianco, V.; Carbone,
C.; Carretero, J.; Casas, R.; Castellano, M.; Cavuoti, S.; Cimatti,
A.; Cledassou, R.; Congedo, G.; Conversi, L.; Copin, Y.; Corcione,
L.; Costille, A.; Cropper, M.; Degaudenzi, H.; Douspis, M.; Dubath,
F.; Dusini, S.; Ealet, A.; Franceschi, E.; Franzetti, P.; Fumana,
M.; Garilli, B.; Gillis, B.; Giocoli, C.; Grazian, A.; Grupp, F.;
Haugan, S. V. H.; Holmes, W.; Hormuth, F.; Jahnke, K.; Kermiche, S.;
Kiessling, A.; Kilbinger, M.; Kümmel, M.; Kunz, M.; Kurki-Suonio,
H.; Laureijs, R.; Ligori, S.; Lilje, P. B.; Lloro, I.; Maiorano, E.;
Mansutti, O.; Marggraf, O.; Markovic, K.; Massey, R.; Medinaceli, E.;
Mei, S.; Meneghetti, M.; Meylan, G.; Moscardini, L.; Niemi, S. M.;
Padilla, C.; Paltani, S.; Pasian, F.; Pedersen, K.; Percival, W. J.;
Pires, S.; Polenta, G.; Poncet, M.; Popa, L.; Pozzetti, L.; Raison,
F.; Rebolo, R.; Roncarelli, M.; Rossetti, E.; Saglia, R.; Sauvage,
M.; Scaramella, R.; Schneider, P.; Seidel, G.; Serrano, S.; Sirignano,
C.; Sirri, G.; Tavagnacco, D.; Taylor, A. N.; Teplitz, H. I.; Tereno,
I.; Toledo-Moreo, R.; Valenziano, L.; Vassallo, T.; Verdoes Kleijn,
G. A.; Wang, Y.; Weller, J.; Wetzstein, M.; Zamorani, G.; Zoubian, J.
Bibcode: 2021PASP..133i4502J
Altcode: 2021arXiv210412752J
The Euclid satellite, to be launched by ESA in 2022, will be a major
instrument for cosmology for the next decades. Euclid is composed of two
instruments: the Visible instrument and the Near Infrared Spectrometer
and Photometer (NISP). In this work, we estimate the implications of
correlated readout noise in the NISP detectors for the final in-flight
flux measurements. Considering the multiple accumulated readout mode,
for which the UTR (Up The Ramp) exposure frames are averaged in
groups, we derive an analytical expression for the noise covariance
matrix between groups in the presence of correlated noise. We also
characterize the correlated readout noise properties in the NISP
engineering-grade detectors using long dark integrations. For
this purpose, we assume a (1/f) α-like noise model
and fit the model parameters to the data, obtaining typical values
of $\sigma ={19.7}_{-0.8}^{+1.1}$ e- Hz-0.5,
${f}_{\mathrm{knee}}=({5.2}_{-1.3}^{+1.8})\times {10}^{-3}\,\mathrm{Hz}$
and $\alpha ={1.24}_{-0.21}^{+0.26}$ . Furthermore, via realistic
simulations and using a maximum likelihood flux estimator we derive
the bias between the input flux and the recovered one. We find that
using our analytical expression for the covariance matrix of the
correlated readout noise we diminish this bias by up to a factor of
four with respect to the white noise approximation for the covariance
matrix. Finally, we conclude that the final bias on the in-flight
NISP flux measurements should still be negligible even in the white
readout noise approximation, which is taken as a baseline for the
Euclid on-board processing to estimate the on-sky flux. * This paper
is published on behalf of the Euclid Consortium.
Title: Euclid Preparation. XIV. The Complete Calibration of the
Color-Redshift Relation (C3R2) Survey: Data Release 3
Authors: Stanford, S. A.; Masters, D.; Darvish, B.; Stern, D.; Cohen,
J. G.; Capak, P.; Hernitschek, N.; Davidzon, I.; Rhodes, J.; Sanders,
D. B.; Mobasher, B.; Castander, F. J.; Paltani, S.; Aghanim, N.;
Amara, A.; Auricchio, N.; Balestra, A.; Bender, R.; Bodendorf, C.;
Bonino, D.; Branchini, E.; Brinchmann, J.; Capobianco, V.; Carbone,
C.; Carretero, J.; Casas, R.; Castellano, M.; Cavuoti, S.; Cimatti, A.;
Cledassou, R.; Conselice, C. J.; Corcione, L.; Costille, A.; Cropper,
M.; Degaudenzi, H.; Douspis, M.; Dubath, F.; Dusini, S.; Fosalba,
P.; Frailis, M.; Franceschi, E.; Franzetti, P.; Fumana, M.; Garilli,
B.; Giocoli, C.; Grupp, F.; Haugan, S. V. H.; Hoekstra, H.; Holmes,
W.; Hormuth, F.; Hudelot, P.; Jahnke, K.; Kiessling, A.; Kilbinger,
M.; Kitching, T.; Kubik, B.; Kümmel, M.; Kunz, M.; Kurki-Suonio,
H.; Laureijs, R.; Ligori, S.; Lilje, P. B.; Lloro, I.; Maiorano, E.;
Marggraf, O.; Markovic, K.; Massey, R.; Meneghetti, M.; Meylan, G.;
Moscardini, L.; Niemi, S. M.; Padilla, C.; Pasian, F.; Pedersen,
K.; Pettorino, V.; Pires, S.; Poncet, M.; Popa, L.; Pozzetti, L.;
Raison, F.; Roncarelli, M.; Rossetti, E.; Saglia, R.; Scaramella, R.;
Schneider, P.; Secroun, A.; Seidel, G.; Serrano, S.; Sirignano, C.;
Sirri, G.; Taylor, A. N.; Teplitz, H. I.; Tereno, I.; Toledo-Moreo,
R.; Valentijn, E. A.; Valenziano, L.; Verdoes Kleijn, G. A.; Wang,
Y.; Zamorani, G.; Zoubian, J.; Brescia, M.; Congedo, G.; Conversi, L.;
Copin, Y.; Kermiche, S.; Kohley, R.; Medinaceli, E.; Mei, S.; Moresco,
M.; Morin, B.; Munari, E.; Polenta, G.; Sureau, F.; Tallada Crespí,
P.; Vassallo, T.; Zacchei, A.; Andreon, S.; Aussel, H.; Baccigalupi,
C.; Balaguera-Antolínez, A.; Baldi, M.; Bardelli, S.; Biviano, A.;
Borsato, E.; Bozzo, E.; Burigana, C.; Cabanac, R.; Camera, S.; Cappi,
A.; Carvalho, C. S.; Casas, S.; Castignani, G.; Colodro-Conde, C.;
Coupon, J.; Courtois, H. M.; Cuby, J. -G.; Da Silva, A.; de la Torre,
S.; Di Ferdinando, D.; Duncan, C. A. J.; Dupac, X.; Fabricius, M.;
Farina, M.; Farrens, S.; Ferreira, P. G.; Finelli, F.; Flose-Reimberg,
P.; Fotopoulou, S.; Galeotta, S.; Ganga, K.; Gillard, W.; Gozaliasl,
G.; Graciá-Carpio, J.; Keihanen, E.; Kirkpatrick, C. C.; Lindholm,
V.; Mainetti, G.; Maino, D.; Martinet, N.; Marulli, F.; Maturi,
M.; Maurogordato, S.; Metcalf, R. B.; Nakajima, R.; Neissner, C.;
Nightingale, J. W.; Nucita, A. A.; Patrizii, L.; Potter, D.; Renzi,
A.; Riccio, G.; Romelli, E.; Sánchez, A. G.; Sapone, D.; Schirmer,
M.; Schultheis, M.; Scottez, V.; Stanco, L.; Tenti, M.; Teyssier,
R.; Torradeflot, F.; Valiviita, J.; Viel, M.; Whittaker, L.; Zucca,
E.; Euclid Collaboration
Bibcode: 2021ApJS..256....9S
Altcode: 2021arXiv210611367S; 2021arXiv210611367E
The Complete Calibration of the Color-Redshift Relation (C3R2)
survey is obtaining spectroscopic redshifts in order to map the
relation between galaxy color and redshift to a depth of i ~ 24.5
(AB). The primary goal is to enable sufficiently accurate photometric
redshifts for Stage IV dark energy projects, particularly Euclid and
the Nancy Grace Roman Space Telescope (Roman), which are designed to
constrain cosmological parameters through weak lensing. We present
676 new high-confidence spectroscopic redshifts obtained by the C3R2
survey in the 2017B-2019B semesters using the DEIMOS, LRIS, and MOSFIRE
multiobject spectrographs on the Keck telescopes. Combined with the
4454 redshifts previously published by this project, the C3R2 survey
has now obtained and published 5130 high-quality galaxy spectra
and redshifts. If we restrict consideration to only the 0.2 <
zp < 2.6 range of interest for the Euclid cosmological
goals, then with the current data release, C3R2 has increased the
spectroscopic redshift coverage of the Euclid color space from 51%
(as reported by Masters et al.) to the current 91%. Once completed and
combined with extensive data collected by other spectroscopic surveys,
C3R2 should provide the spectroscopic calibration set needed to enable
photometric redshifts to meet the cosmology requirements for Euclid,
and make significant headway toward solving the problem for Roman.
Title: SSTRED: Data- and metadata-processing pipeline for CHROMIS
and CRISP
Authors: Löfdahl, Mats G.; Hillberg, Tomas; de la Cruz Rodríguez,
Jaime; Vissers, Gregal; Andriienko, Oleksii; Scharmer, Göran B.;
Haugan, Stein V. H.; Fredvik, Terje
Bibcode: 2021A&A...653A..68L
Altcode: 2018arXiv180403030L
Context. Data from ground-based, high-resolution solar telescopes
can only be used for science with calibrations and processing, which
requires detailed knowledge about the instrumentation. Space-based
solar telescopes provide science-ready data, which are easier to
work with for researchers whose expertise is in the interpretation of
data. Recently, data-processing pipelines for ground-based instruments
have been constructed.
Aims: We aim to provide observers
with a user-friendly data pipeline for data from the Swedish 1-meter
Solar Telescope (SST) that delivers science-ready data together with
the metadata needed for proper interpretation and archiving.
Methods: We briefly describe the CHROMospheric Imaging Spectrometer
(CHROMIS) instrument, including its (pre)filters, as well as recent
upgrades to the CRisp Imaging SpectroPolarimeter (CRISP) prefilters and
polarization optics. We summarize the processing steps from raw data
to science-ready data cubes in FITS files. We report calibrations
and compensations for data imperfections in detail. Misalignment
of Ca II data due to wavelength-dependent dispersion is identified,
characterized, and compensated for. We describe intensity calibrations
that remove or reduce the effects of filter transmission profiles
as well as solar elevation changes. We present REDUX, a new version
of the MOMFBD image restoration code, with multiple enhancements and
new features. It uses projective transforms for the registration of
multiple detectors. We describe how image restoration is used with
CRISP and CHROMIS data. The science-ready output is delivered in FITS
files, with metadata compliant with the SOLARNET recommendations. Data
cube coordinates are specified within the World Coordinate System
(WCS). Cavity errors are specified as distortions of the WCS wavelength
coordinate with an extension of existing WCS notation. We establish
notation for specifying the reference system for Stokes vectors with
reference to WCS coordinate directions. The CRIsp SPectral EXplorer
(CRISPEX) data-cube browser has been extended to accept SSTRED output
and to take advantage of the SOLARNET metadata.
Results: SSTRED
is a mature data-processing pipeline for imaging instruments, developed
and used for the SST/CHROMIS imaging spectrometer and the SST/CRISP
spectropolarimeter. SSTRED delivers well-characterized, science-ready,
archival-quality FITS files with well-defined metadata. The SSTRED
code, as well as REDUX and CRISPEX, is freely available through git
repositories.
Title: Euclid : Effects of sample covariance on the number counts
of galaxy clusters
Authors: Fumagalli, A.; Saro, A.; Borgani, S.; Castro, T.; Costanzi,
M.; Monaco, P.; Munari, E.; Sefusatti, E.; Amara, A.; Auricchio, N.;
Balestra, A.; Bodendorf, C.; Bonino, D.; Branchini, E.; Brinchmann,
J.; Capobianco, V.; Carbone, C.; Castellano, M.; Cavuoti, S.; Cimatti,
A.; Cledassou, R.; Conselice, C. J.; Corcione, L.; Costille, A.;
Cropper, M.; Degaudenzi, H.; Douspis, M.; Dubath, F.; Dusini, S.;
Ealet, A.; Fosalba, P.; Franceschi, E.; Franzetti, P.; Fumana, M.;
Garilli, B.; Giocoli, C.; Grupp, F.; Guzzo, L.; Haugan, S. V. H.;
Hoekstra, H.; Holmes, W.; Hormuth, F.; Jahnke, K.; Kiessling, A.;
Kilbinger, M.; Kitching, T.; Kümmel, M.; Kunz, M.; Kurki-Suonio,
H.; Laureijs, R.; Lilje, P. B.; Lloro, I.; Maiorano, E.; Marggraf,
O.; Markovic, K.; Massey, R.; Meneghetti, M.; Meylan, G.; Moscardini,
L.; Niemi, S. M.; Padilla, C.; Paltani, S.; Pasian, F.; Pedersen, K.;
Pettorino, V.; Pires, S.; Poncet, M.; Popa, L.; Pozzetti, L.; Raison,
F.; Rhodes, J.; Roncarelli, M.; Rossetti, E.; Saglia, R.; Scaramella,
R.; Schneider, P.; Secroun, A.; Seidel, G.; Serrano, S.; Sirignano,
C.; Sirri, G.; Taylor, A. N.; Tereno, I.; Toledo-Moreo, R.; Valentijn,
E. A.; Valenziano, L.; Wang, Y.; Weller, J.; Zamorani, G.; Zoubian,
J.; Brescia, M.; Congedo, G.; Conversi, L.; Mei, S.; Moresco, M.;
Vassallo, T.
Bibcode: 2021A&A...652A..21F
Altcode: 2021arXiv210208914F
Aims: We investigate the contribution of shot-noise and sample
variance to uncertainties in the cosmological parameter constraints
inferred from cluster number counts, in the context of the Euclid
survey.
Methods: By analysing 1000 Euclid-like light cones,
produced with the PINOCCHIO approximate method, we validated the
analytical model of Hu & Kravtsov (2003, ApJ, 584, 702) for the
covariance matrix, which takes into account both sources of statistical
error. Then, we used such a covariance to define the likelihood function
that is better equipped to extract cosmological information from cluster
number counts at the level of precision that will be reached by the
future Euclid photometric catalogs of galaxy clusters. We also studied
the impact of the cosmology dependence of the covariance matrix on
the parameter constraints.
Results: The analytical covariance
matrix reproduces the variance measured from simulations within the
10 percent; such a difference has no sizeable effect on the error of
cosmological parameter constraints at this level of statistics. Also,
we find that the Gaussian likelihood with full covariance is the only
model that provides an unbiased inference of cosmological parameters
without underestimating the errors, and that the cosmology-dependence of
the covariance must be taken into account. This paper is published
on behalf of the Euclid Consortium.
Title: Euclid: Forecasts for k-cut 3×2 Point Statistics
Authors: Taylor, Peter L.; Kitching, T.; Cardone, V. F.; Ferté,
A.; Huff, E. M.; Bernardeau, F.; Rhodes, J.; Deshpande, A. C.;
Tutusaus, I.; Pourtsidou, Alkistis; Camera, S.; Carbone, C.; Casas,
S.; Martinelli, M.; Pettorino, V.; Sakr, Z.; Sapone, D.; Yankelevich,
V.; Auricchio, N.; Balestra, A.; Bodendorf, C.; Bonino, D.; Boucaud,
A.; Branchini, Enzo; Brescia, M.; Capobianco, V.; Carretero, J.;
Castellano, M.; Cavuoti, S.; Cimatti, A.; Cledassou, R.; Congedo, G.;
Conversi, L.; Corcione, L.; Cropper, Mark; Franceschi, E.; Garilli,
B.; Gillis, B.; Giocoli, C.; Guzzo, L.; Haugan, S. V. H.; Holmes, W.;
Hormuth, F.; Jahnke, Knud; Kermiche, S.; Kilbinger, M.; Kunz, M.;
Kurki-Suonio, H.; Ligori, S.; Lilje, Per B.; Lloro, I.; Marggraf,
O.; Markovic, K.; Massey, R.; Mei, S.; Medinaceli, E.; Meneghetti,
M.; Meylan, G.; Moresco, M.; Morin, B.; Moscardini, Lauro; Niemi,
S.; Padilla, C.; Pasian, F.; Paltani, S.; Pedersen, K.; Pires, S.;
Percival, Will J.; Polenta, G.; Poncet, M.; Popa, L.; Raison, F.;
Roncarelli, M.; Rossetti, E.; Saglia, R.; Schneider, Peter; Secroun,
A.; Seidel, G.; Serrano, S.; Sirignano, C.; Sirri, G.; Sureau, F.;
Crespí, P. Tallada; Tavagnacco, D.; Taylor, A. N.; Teplitz, H. I.;
Tereno, I.; Toledo-Moreo, R.; Valentijn, E. A.; Valenziano, L.;
Vassallo, T.; Wang, Yun; Weller, Jochen; Zacchei, A.; Zoubian, J.
Bibcode: 2021OJAp....4E...6T
Altcode: 2020arXiv201204672T
Modelling uncertainties at small scales, i.e. high $k$ in the power
spectrum $P(k)$, due to baryonic feedback, nonlinear structure growth
and the fact that galaxies are biased tracers poses a significant
obstacle to fully leverage the constraining power of the {\it Euclid}
wide-field survey. $k$-cut cosmic shear has recently been proposed
as a method to optimally remove sensitivity to these scales while
preserving usable information. In this paper we generalise the $k$-cut
cosmic shear formalism to $3 \times 2$ point statistics and estimate
the loss of information for different $k$-cuts in a $3 \times 2$
point analysis of the {\it Euclid} data. Extending the Fisher matrix
analysis of~\citet{blanchard2019euclid}, we assess the degradation in
constraining power for different $k$-cuts. We work in the idealised
case and assume the galaxy bias is linear, the covariance is Gaussian,
while neglecting uncertainties due to photo-z errors and baryonic
feedback. We find that taking a $k$-cut at $2.6 \ h \ {\rm Mpc} ^{-1}$
yields a dark energy Figure of Merit (FOM) of 1018. This is comparable
to taking a weak lensing cut at $\ell = 5000$ and a galaxy clustering
and galaxy-galaxy lensing cut at $\ell = 3000$ in a traditional $3
\times 2$ point analysis. We also find that the fraction of the
observed galaxies used in the photometric clustering part of the
analysis is one of the main drivers of the FOM. Removing $50 \% \
(90 \%)$ of the clustering galaxies decreases the FOM by $19 \% \
(62 \%)$. Given that the FOM depends so heavily on the fraction of
galaxies used in the clustering analysis, extensive efforts should be
made to handle the real-world systematics present when extending the
analysis beyond the luminous red galaxy (LRG) sample.
Title: Euclid preparation. XI. Mean redshift determination from
galaxy redshift probabilities for cosmic shear tomography
Authors: Euclid Collaboration; Ilbert, O.; de la Torre, S.;
Martinet, N.; Wright, A. H.; Paltani, S.; Laigle, C.; Davidzon, I.;
Jullo, E.; Hildebrandt, H.; Masters, D. C.; Amara, A.; Conselice,
C. J.; Andreon, S.; Auricchio, N.; Azzollini, R.; Baccigalupi,
C.; Balaguera-Antolínez, A.; Baldi, M.; Balestra, A.; Bardelli,
S.; Bender, R.; Biviano, A.; Bodendorf, C.; Bonino, D.; Borgani,
S.; Boucaud, A.; Bozzo, E.; Branchini, E.; Brescia, M.; Burigana,
C.; Cabanac, R.; Camera, S.; Capobianco, V.; Cappi, A.; Carbone,
C.; Carretero, J.; Carvalho, C. S.; Casas, S.; Castander, F. J.;
Castellano, M.; Castignani, G.; Cavuoti, S.; Cimatti, A.; Cledassou,
R.; Colodro-Conde, C.; Congedo, G.; Conversi, L.; Copin, Y.; Corcione,
L.; Costille, A.; Coupon, J.; Courtois, H. M.; Cropper, M.; Cuby,
J.; Da Silva, A.; Degaudenzi, H.; Di Ferdinando, D.; Dubath, F.;
Duncan, C.; Dupac, X.; Dusini, S.; Ealet, A.; Fabricius, M.; Farrens,
S.; Ferreira, P. G.; Finelli, F.; Fosalba, P.; Fotopoulou, S.;
Franceschi, E.; Franzetti, P.; Galeotta, S.; Garilli, B.; Gillard,
W.; Gillis, B.; Giocoli, C.; Gozaliasl, G.; Graciá-Carpio, J.;
Grupp, F.; Guzzo, L.; Haugan, S. V. H.; Holmes, W.; Hormuth, F.;
Jahnke, K.; Keihanen, E.; Kermiche, S.; Kiessling, A.; Kirkpatrick,
C. C.; Kunz, M.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro,
I.; Maino, D.; Maiorano, E.; Marggraf, O.; Markovic, K.; Marulli, F.;
Massey, R.; Maturi, M.; Mauri, N.; Maurogordato, S.; McCracken, H. J.;
Medinaceli, E.; Mei, S.; Metcalf, R. Benton; Moresco, M.; Morin, B.;
Moscardini, L.; Munari, E.; Nakajima, R.; Neissner, C.; Niemi, S.;
Nightingale, J.; Padilla, C.; Pasian, F.; Patrizii, L.; Pedersen, K.;
Pello, R.; Pettorino, V.; Pires, S.; Polenta, G.; Poncet, M.; Popa,
L.; Potter, D.; Pozzetti, L.; Raison, F.; Renzi, A.; Rhodes, J.;
Riccio, G.; Romelli, E.; Roncarelli, M.; Rossetti, E.; Saglia, R.;
Sánchez, A. G.; Sapone, D.; Schneider, P.; Schrabback, T.; Scottez,
V.; Secroun, A.; Seidel, G.; Serrano, S.; Sirignano, C.; Sirri, G.;
Stanco, L.; Sureau, F.; Tallada Crespá, P.; Tenti, M.; Teplitz,
H. I.; Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.; Tramacere, A.;
Valentijn, E. A.; Valenziano, L.; Valiviita, J.; Vassallo, T.; Wang,
Y.; Welikala, N.; Weller, J.; Whittaker, L.; Zacchei, A.; Zamorani,
G.; Zoubian, J.; Zucca, E.
Bibcode: 2021A&A...647A.117E
Altcode: 2021arXiv210102228E
The analysis of weak gravitational lensing in wide-field imaging surveys
is considered to be a major cosmological probe of dark energy. Our
capacity to constrain the dark energy equation of state relies on an
accurate knowledge of the galaxy mean redshift ⟨z⟩. We investigate
the possibility of measuring ⟨z⟩ with an accuracy better than
0.002 (1 + z) in ten tomographic bins spanning the redshift interval
0.2 < z < 2.2, the requirements for the cosmic shear analysis
of Euclid. We implement a sufficiently realistic simulation in order
to understand the advantages and complementarity, as well as the
shortcomings, of two standard approaches: the direct calibration of
⟨z⟩ with a dedicated spectroscopic sample and the combination
of the photometric redshift probability distribution functions
(zPDFs) of individual galaxies. We base our study on the Horizon-AGN
hydrodynamical simulation, which we analyse with a standard galaxy
spectral energy distribution template-fitting code. Such a procedure
produces photometric redshifts with realistic biases, precisions,
and failure rates. We find that the current Euclid design for direct
calibration is sufficiently robust to reach the requirement on the mean
redshift, provided that the purity level of the spectroscopic sample is
maintained at an extremely high level of > 99.8%. The zPDF approach
can also be successful if the zPDF is de-biased using a spectroscopic
training sample. This approach requires deep imaging data but is weakly
sensitive to spectroscopic redshift failures in the training sample. We
improve the de-biasing method and confirm our finding by applying it
to real-world weak-lensing datasets (COSMOS and KiDS+VIKING-450).
Title: Euclid preparation. X. The Euclid photometric-redshift
challenge
Authors: Euclid Collaboration; Desprez, G.; Paltani, S.; Coupon, J.;
Almosallam, I.; Alvarez-Ayllon, A.; Amaro, V.; Brescia, M.; Brodwin,
M.; Cavuoti, S.; De Vicente-Albendea, J.; Fotopoulou, S.; Hatfield,
P. W.; Hartley, W. G.; Ilbert, O.; Jarvis, M. J.; Longo, G.; Rau,
M. M.; Saha, R.; Speagle, J. S.; Tramacere, A.; Castellano, M.;
Dubath, F.; Galametz, A.; Kuemmel, M.; Laigle, C.; Merlin, E.; Mohr,
J. J.; Pilo, S.; Salvato, M.; Andreon, S.; Auricchio, N.; Baccigalupi,
C.; Balaguera-Antolínez, A.; Baldi, M.; Bardelli, S.; Bender, R.;
Biviano, A.; Bodendorf, C.; Bonino, D.; Bozzo, E.; Branchini, E.;
Brinchmann, J.; Burigana, C.; Cabanac, R.; Camera, S.; Capobianco,
V.; Cappi, A.; Carbone, C.; Carretero, J.; Carvalho, C. S.; Casas, R.;
Casas, S.; Castander, F. J.; Castignani, G.; Cimatti, A.; Cledassou,
R.; Colodro-Conde, C.; Congedo, G.; Conselice, C. J.; Conversi, L.;
Copin, Y.; Corcione, L.; Courtois, H. M.; Cuby, J. -G.; Da Silva,
A.; de la Torre, S.; Degaudenzi, H.; Di Ferdinando, D.; Douspis, M.;
Duncan, C. A. J.; Dupac, X.; Ealet, A.; Fabbian, G.; Fabricius, M.;
Farrens, S.; Ferreira, P. G.; Finelli, F.; Fosalba, P.; Fourmanoit, N.;
Frailis, M.; Franceschi, E.; Fumana, M.; Galeotta, S.; Garilli, B.;
Gillard, W.; Gillis, B.; Giocoli, C.; Gozaliasl, G.; Graciá-Carpio,
J.; Grupp, F.; Guzzo, L.; Hailey, M.; Haugan, S. V. H.; Holmes, W.;
Hormuth, F.; Humphrey, A.; Jahnke, K.; Keihanen, E.; Kermiche, S.;
Kilbinger, M.; Kirkpatrick, C. C.; Kitching, T. D.; Kohley, R.; Kubik,
B.; Kunz, M.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro, I.;
Maino, D.; Maiorano, E.; Marggraf, O.; Markovic, K.; Martinet, N.;
Marulli, F.; Massey, R.; Maturi, M.; Mauri, N.; Maurogordato, S.;
Medinaceli, E.; Mei, S.; Meneghetti, M.; Metcalf, R. Benton; Meylan,
G.; Moresco, M.; Moscardini, L.; Munari, E.; Niemi, S.; Padilla,
C.; Pasian, F.; Patrizii, L.; Pettorino, V.; Pires, S.; Polenta, G.;
Poncet, M.; Popa, L.; Potter, D.; Pozzetti, L.; Raison, F.; Renzi,
A.; Rhodes, J.; Riccio, G.; Rossetti, E.; Saglia, R.; Sapone, D.;
Schneider, P.; Scottez, V.; Secroun, A.; Serrano, S.; Sirignano, C.;
Sirri, G.; Stanco, L.; Stern, D.; Sureau, F.; Tallada Crespí, P.;
Tavagnacco, D.; Taylor, A. N.; Tenti, M.; Tereno, I.; Toledo-Moreo, R.;
Torradeflot, F.; Valenziano, L.; Valiviita, J.; Vassallo, T.; Viel,
M.; Wang, Y.; Welikala, N.; Whittaker, L.; Zacchei, A.; Zamorani,
G.; Zoubian, J.; Zucca, E.
Bibcode: 2020A&A...644A..31E
Altcode: 2020arXiv200912112E
Forthcoming large photometric surveys for cosmology require precise and
accurate photometric redshift (photo-z) measurements for the success
of their main science objectives. However, to date, no method has
been able to produce photo-zs at the required accuracy using only the
broad-band photometry that those surveys will provide. An assessment
of the strengths and weaknesses of current methods is a crucial step
in the eventual development of an approach to meet this challenge. We
report on the performance of 13 photometric redshift code single
value redshift estimates and redshift probability distributions
(PDZs) on a common set of data, focusing particularly on the 0.2 -
2.6 redshift range that the Euclid mission will probe. We designed
a challenge using emulated Euclid data drawn from three photometric
surveys of the COSMOS field. The data was divided into two samples:
one calibration sample for which photometry and redshifts were provided
to the participants; and the validation sample, containing only the
photometry to ensure a blinded test of the methods. Participants were
invited to provide a redshift single value estimate and a PDZ for each
source in the validation sample, along with a rejection flag that
indicates the sources they consider unfit for use in cosmological
analyses. The performance of each method was assessed through a
set of informative metrics, using cross-matched spectroscopic and
highly-accurate photometric redshifts as the ground truth. We show that
the rejection criteria set by participants are efficient in removing
strong outliers, that is to say sources for which the photo-z deviates
by more than 0.15(1 + z) from the spectroscopic-redshift (spec-z). We
also show that, while all methods are able to provide reliable single
value estimates, several machine-learning methods do not manage to
produce useful PDZs. We find that no machine-learning method provides
good results in the regions of galaxy color-space that are sparsely
populated by spectroscopic-redshifts, for example z > 1. However
they generally perform better than template-fitting methods at low
redshift (z < 0.7), indicating that template-fitting methods do not
use all of the information contained in the photometry. We introduce
metrics that quantify both photo-z precision and completeness of the
samples (post-rejection), since both contribute to the final figure
of merit of the science goals of the survey (e.g., cosmic shear from
Euclid). Template-fitting methods provide the best results in these
metrics, but we show that a combination of template-fitting results
and machine-learning results with rejection criteria can outperform
any individual method. On this basis, we argue that further work
in identifying how to best select between machine-learning and
template-fitting approaches for each individual galaxy should be
pursued as a priority.
Title: Euclid: Forecast constraints on the cosmic distance duality
relation with complementary external probes
Authors: Martinelli, M.; Martins, C. J. A. P.; Nesseris, S.; Sapone,
D.; Tutusaus, I.; Avgoustidis, A.; Camera, S.; Carbone, C.; Casas,
S.; Ilić, S.; Sakr, Z.; Yankelevich, V.; Auricchio, N.; Balestra, A.;
Bodendorf, C.; Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann, J.;
Capobianco, V.; Carretero, J.; Castellano, M.; Cavuoti, S.; Cledassou,
R.; Congedo, G.; Conversi, L.; Corcione, L.; Dubath, F.; Ealet, A.;
Frailis, M.; Franceschi, E.; Fumana, M.; Garilli, B.; Gillis, B.;
Giocoli, C.; Grupp, F.; Haugan, S. V. H.; Holmes, W.; Hormuth, F.;
Jahnke, K.; Kermiche, S.; Kilbinger, M.; Kitching, T. D.; Kubik,
B.; Kunz, M.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lloro,
I.; Marggraf, O.; Markovic, K.; Massey, R.; Mei, S.; Meneghetti,
M.; Meylan, G.; Moscardini, L.; Niemi, S.; Padilla, C.; Paltani, S.;
Pasian, F.; Pettorino, V.; Pires, S.; Polenta, G.; Poncet, M.; Popa,
L.; Pozzetti, L.; Raison, F.; Rhodes, J.; Roncarelli, M.; Saglia, R.;
Schneider, P.; Secroun, A.; Serrano, S.; Sirignano, C.; Sirri, G.;
Sureau, F.; Taylor, A. N.; Tereno, I.; Toledo-Moreo, R.; Valenziano,
L.; Vassallo, T.; Wang, Y.; Welikala, N.; Weller, J.; Zacchei, A.
Bibcode: 2020A&A...644A..80M
Altcode: 2020arXiv200716153M
Context. In metric theories of gravity with photon number conservation,
the luminosity and angular diameter distances are related via the
Etherington relation, also known as the distance duality relation
(DDR). A violation of this relation would rule out the standard
cosmological paradigm and point to the presence of new physics.
Aims: We quantify the ability of Euclid, in combination with
contemporary surveys, to improve the current constraints on deviations
from the DDR in the redshift range 0 < z < 1.6.
Methods:
We start with an analysis of the latest available data, improving
previously reported constraints by a factor of 2.5. We then present
a detailed analysis of simulated Euclid and external data products,
using both standard parametric methods (relying on phenomenological
descriptions of possible DDR violations) and a machine learning
reconstruction using genetic algorithms.
Results: We find that
for parametric methods Euclid can (in combination with external probes)
improve current constraints by approximately a factor of six, while
for non-parametric methods Euclid can improve current constraints
by a factor of three.
Conclusions: Our results highlight the
importance of surveys like Euclid in accurately testing the pillars of
the current cosmological paradigm and constraining physics beyond the
standard cosmological model. This paper is published on behalf
of the Euclid Consortium.
Title: SOLARNET Metadata Recommendations for Solar Observations
Authors: Haugan, Stein Vidar Hagfors; Fredvik, Terje
Bibcode: 2020arXiv201112139H
Altcode: 2020arXiv201112139V
Metadata descriptions of Solar observations have so far only been
standardized for space-based observations, but the standards have
been mostly within a single space mission at a time, at times with
significant differences between different mission standards. In the
context of ground-based Solar observations, data has typically not been
made freely available to the general research community, resulting in an
even greater lack of standards for metadata descriptions. This situation
makes it difficult to construct multi-instrument archives/virtual
observatories with anything more than the most basic metadata available
for searching, as well as making it difficult to write generic software
for instrument-agnostic data analysis. This document describes the
metadata recommendations developed under the SOLARNET EU project,
which aims foster more collaboration and data sharing between both
ground-based and space-based Solar observatories. The recommendations
will be followed by data pipelines developed under the SOLARNET
project as well as e.g. the Solar Orbiter SPICE pipeline and the SST
CHROMIS/CRISP common pipeline. These recommendations are meant to
function as a common reference to which even existing diverse data
sets may be related, for ingestion into solar virtual observatories
and for analysis by generic software.
Title: The Solar Orbiter SPICE instrument. An extreme UV imaging
spectrometer
Authors: SPICE Consortium; Anderson, M.; Appourchaux, T.; Auchère, F.;
Aznar Cuadrado, R.; Barbay, J.; Baudin, F.; Beardsley, S.; Bocchialini,
K.; Borgo, B.; Bruzzi, D.; Buchlin, E.; Burton, G.; Büchel, V.;
Caldwell, M.; Caminade, S.; Carlsson, M.; Curdt, W.; Davenne, J.;
Davila, J.; Deforest, C. E.; Del Zanna, G.; Drummond, D.; Dubau,
J.; Dumesnil, C.; Dunn, G.; Eccleston, P.; Fludra, A.; Fredvik, T.;
Gabriel, A.; Giunta, A.; Gottwald, A.; Griffin, D.; Grundy, T.; Guest,
S.; Gyo, M.; Haberreiter, M.; Hansteen, V.; Harrison, R.; Hassler,
D. M.; Haugan, S. V. H.; Howe, C.; Janvier, M.; Klein, R.; Koller,
S.; Kucera, T. A.; Kouliche, D.; Marsch, E.; Marshall, A.; Marshall,
G.; Matthews, S. A.; McQuirk, C.; Meining, S.; Mercier, C.; Morris,
N.; Morse, T.; Munro, G.; Parenti, S.; Pastor-Santos, C.; Peter, H.;
Pfiffner, D.; Phelan, P.; Philippon, A.; Richards, A.; Rogers, K.;
Sawyer, C.; Schlatter, P.; Schmutz, W.; Schühle, U.; Shaughnessy,
B.; Sidher, S.; Solanki, S. K.; Speight, R.; Spescha, M.; Szwec, N.;
Tamiatto, C.; Teriaca, L.; Thompson, W.; Tosh, I.; Tustain, S.; Vial,
J. -C.; Walls, B.; Waltham, N.; Wimmer-Schweingruber, R.; Woodward,
S.; Young, P.; de Groof, A.; Pacros, A.; Williams, D.; Müller, D.
Bibcode: 2020A&A...642A..14S
Altcode: 2019arXiv190901183A; 2019arXiv190901183S
Aims: The Spectral Imaging of the Coronal Environment (SPICE)
instrument is a high-resolution imaging spectrometer operating at
extreme ultraviolet wavelengths. In this paper, we present the concept,
design, and pre-launch performance of this facility instrument on the
ESA/NASA Solar Orbiter mission.
Methods: The goal of this paper
is to give prospective users a better understanding of the possible
types of observations, the data acquisition, and the sources that
contribute to the instrument's signal.
Results: The paper
discusses the science objectives, with a focus on the SPICE-specific
aspects, before presenting the instrument's design, including optical,
mechanical, thermal, and electronics aspects. This is followed by a
characterisation and calibration of the instrument's performance. The
paper concludes with descriptions of the operations concept and data
processing.
Conclusions: The performance measurements of the
various instrument parameters meet the requirements derived from the
mission's science objectives. The SPICE instrument is ready to perform
measurements that will provide vital contributions to the scientific
success of the Solar Orbiter mission.
Title: A virtual appliance as proxy pipeline for the Solar
Orbiter/Metis coronagraph
Authors: Pancrazzi, M.; Straus, T.; Andretta, V.; Spadaro, D.; Haugan,
S. V.; de Groof, A.; Carr, R.; Focardi, M.; Nicolini, G.; Landini,
F.; Baccani, C.; Romoli, M.; Antonucci, E.
Bibcode: 2016SPIE.9913E..4LP
Altcode:
Metis is the coronagraph on board Solar Orbiter, the ESA mission devoted
to the study of the Sun that will be launched in October 2018. Metis is
designed to perform imaging of the solar corona in the UV at 121.6 nm
and in the visible range where it will accomplish polarimetry studies
thanks to a variable retarder plate. Due to mission constraints, the
telemetry downlink on the spacecraft will be limited and data will be
downloaded with delays that could reach, in the worst case, several
months. In order to have a quick overview on the ongoing operations
and to check the safety of the 10 instruments on board, a high-priority
downlink channel has been foreseen to download a restricted amount of
data. These so-called Low Latency Data will be downloaded daily and,
since they could trigger possible actions, they have to be quickly
processed on ground as soon as they are delivered. To do so, a proper
processing pipeline has to be developed by each instrument. This
tool will then be integrated in a single system at the ESA Science
Operation Center that will receive the downloaded data by the Mission
Operation Center. This paper will provide a brief overview of the on
board processing and data produced by Metis and it will describe the
proxy-pipeline currently under development to deal with the Metis
low-latency data.
Title: Tools for the evaluation of the possibilities of using parallax
measurements of gravitationally lensed sources
Authors: Haugan, Stein Vidar Hagfors
Bibcode: 2008PhDT.......291H
Altcode:
No abstract at ADS
Title: 10 years of SOHO
Authors: Fleck, Bernhard; Müller, Daniel; Haugan, Stein; Sánchez
Duarte, Luis; Siili, Tero; Gurman, Joseph B.
Bibcode: 2006ESABu.126...24F
Altcode:
Since its launch on 2 December 1995, SOHO has revolutionised
our understanding of the Sun. It has provided the first images of
structures and flows below the Sun's surface and of activity on the
far side. SOHO has revealed the Sun's extremely dynamic atmosphere,
provided evidence for the transfer of magnetic energy from the surface
the outer solar atmosphere, the corona, through a "magnetic carpet",
and identified the source regions of the fast solar wind. It has
revolutionised our understanding of solar-terrestrial relations and
dramatically improved our space weather-forecasting by its continuous
stream of images covering the atmosphere, extended corona and far
side. The findings are documented in an impressive number of scientific
publications: over 2500 papers in refereed journals since launch,
representing the work of over 2300 individual scientists. At the
same time, SOHO's easily accessible, spectacular data and fundamental
scientific results have captured the imagination of the space science
community and the general public alike. As a byproduct of the efforts
to provide real-time data to the public, amateurs now dominate SOHO's
discovery of over 1100 Sungrazing comets.
Title: Space Weather Effects on SOHO and its Leading Role as a Space
Weather Wãtchdog
Authors: Brekke, P.; Fleck, B.; Haugan, S. V.; van Overbeek, T.;
Schweitzer, H.; Simonin, B.
Bibcode: 2005mcsp.conf...83B
Altcode:
No abstract at ADS
Title: Coordinating with SOHO
Authors: Haugan, Stein V. H.
Bibcode: 2005AdSpR..36.1557H
Altcode:
I describe how to maximise the chances of achieving a successful
coordinated observation campaign together with SOHO instruments (and
TRACE). The ground rules, common pitfalls, useful resources and some
essential “tricks of the trade” are covered. The most important
hints are: start early, make contact with the instrument teams and
the SOCs (soc@soc.nascom.nasa.gov), ask whenever in doubt, check the
calendar, and be specific.
Title: Coordinating with SOHO
Authors: Haugan, S. V. H.
Bibcode: 2004cosp...35.3150H
Altcode: 2004cosp.meet.3150H
I will describe how to maximise the chances of achieving a successful
coordinated observation campaign together with SOHO instruments (and
TRACE). The ground rules, common pitfalls, useful resources and some
essential "tricks of the trade" will be covered. The most important
hints are: start early, make contact with the instrument teams, ask
the SOCs when in doubt (soc@soc.nascom.nasa.gov), check our calendar,
and be specific.
Title: Variability and dynamic state of active region loops
Authors: Fredvik, T.; Kjeldseth-Moe, O.; Haugan, S. V. H.; Brekke,
P.; Gurman, J. B.; Wilhelm, K.
Bibcode: 2002AdSpR..30..635F
Altcode:
A set of 218 consecutive CDS rasters taken at the solar limb on October
26-28 1999 has been used to investigate the variability and plasma
dynamics of active region loops. Each raster contains simultaneous
images in 6 different lines, covering the full temperature range of
CDS, 10 000 K (He I) to 2.7 MK (Fe XVI). Activity is seen to go on
without breaks at temperatures below 1 MK for the full 39 hours of the
series. Transition region loops or extended sections of loops, 50-200
Mm long, appear and disappear in intervals as short as 11 minutes,
the observing cadence. In the corona the emission is less variable,
but significant changes are seen. Measured Doppler shifts correspond
to typical plasma velocities of 20 km s -1 to 100 km
s -1, at temperatures 10 000 K to 450 000 K, and siphon
flows may occur in some of the loops. High velocities are frequently
seen where the emitted intensities are weak, often on the outer edges
of loops as defined in that particular spectral line. At coronal
temperatures, 1 MK and higher, systematic loop velocities occur only
occasionally. Simultaneous observations with EIT and SUMER were made
during part of the raster series and are compared with the CDS result.
Title: The Sun During The Ulysses Fast Latitude Scan and Northern
Polar Pass As Seen By Soho
Authors: Fleck, B.; Brekke, P.; Haugan, S. V. H.
Bibcode: 2002EGSGA..27.3839F
Altcode:
In 2001, during the Ulysses fast latitude scan (January - September)
and second north- ern polar pass (September - December), the Sun showed
a remarkable resurgence of solar activity after its rapid drop-off
following the activity maximum in the summer of 2000. In early April
active region 9393, the largest active region of the current cycle,
produced a series of events, among them the biggest X-ray flare on
record. In the fall there were three severe proton storms, one of them
the third largest on record since measurements began in 1976. It is
interesting to note that five out of the eight proton storms with flux
densities greater than 10,000 cm-2 s-1 sr-1 (>10 MeV) since 1976
occurred in cycle 23, and three of these five in 2001. The overall
change in solar ac- tivity in 2001 will be reviewed and some of the
most dramatic events from that year discussed.
Title: Space Weather Effects on SOHO
Authors: Brekke, P.; Fleck, B.; Haugan, S.; Schweitzer, H.; Chaloupy,
M.
Bibcode: 2002cosp...34E2156B
Altcode: 2002cosp.meetE2156B
Since its launch on 2 December 1995, the Solar and Heliospheric
Observatory (SOHO) has provided an unparalleled breadth and depth of
information about the Sun, from its interior, through the hot and
dynamic atmosphere, and out to the solar wind. SOHO is in a halo
orbit around L1 Lagrangian point where it views the Sun 24 hours a
day. Thus, it is situated outside the Earth's protective magnetosphere
which shields other satellites from high energy particles from the
Sun. We present a summary of the observed effects on the instruments
and electronics on SOHO throughout the mission. In particular we will
focus on a number of large particle events during the recent years
while the Sun was approaching maximum activity, and how they affected
both the scientific data as well as hardware components.
Title: Anomalous Line Shifts on the SOHO/CDS NIS Detector
Authors: Haugan, S. V. H.
Bibcode: 2001IAUS..203..396H
Altcode:
Observations with the SOHO/CDS NIS detector prior to the recovery
of SOHO show strong correlations between line shifts and local
intensity gradients along the slit. The most plausible explanation
is an elliptical, tilted point spread function inducing anomalous
line shifts. This must be taken into account when interpreting NIS
observations with strong intensity gradients. The optical properties
of SOHO/CDS changed quite significantly during the time period when
SOHO was out of control. Initial results from a similar analysis of
post-recovery data will also be presented.
Title: Observed Variability and Dynamics of Active Region Loops
Authors: Haugan, S. V. H.; Brekke, P.; Fredvik, T.; Kjeldseth-Moe,
O.; Wilhelm, K.; Gurman, J. B.
Bibcode: 2000SPD....31.0205H
Altcode: 2000BAAS...32..811H
A series of 218 rasters taken with the Coronal Diagnostic Spectrometer
(CDS) on SOHO demonstrates the strong time variability and
dynamical state of the plasma in active region loops at transition
region temperatures, i.e. 10 000 K to 500 000 K, first reported
by Kjeldseth-Moe and Brekke (1998). The continuous raster series,
which covered 39 hours, show how transition region loops or sections
of loops, 50-200 Mm in length, appear and disappear in intervals as
short as 10 minutes, the observing cadence. At the same temperatures
plasma velocities of 20 km s-1 to 100 km s-1
are indicated from observed Doppler shifts. Siphon flows may occur in
some of the loops, but in other loops patterns are less obvious. High
velocities are frequently seen where the emitted intensities are weak,
often on the ``outside'' of the loops as defined by the emission in
that particular spectral line. At coronal temperatures the emission
is less time variable, but significant changes are seen. Systematic
loop velocities occur only occasionally in the corona. Simultaneous
observations with EIT and SUMER were made during part of the raster
series and is compared with the CDS result.
Title: Four years of SOHO discoveries - some highlights.
Authors: Fleck, B.; Brekke, P.; Haugan, S.; Duarte, L. S.; Domingo,
V.; Gurman, J. B.; Poland, A. I.
Bibcode: 2000ESABu.102...68F
Altcode:
Analysis of the helioseismic data from SOHO has shed new light on
solar and heliosheric physics: the structure and dynamics of the
solar interior, the heating and dynamics of the solar corona, and the
acceleration and composition of the solar wind.
Title: Structure and Dynamics in the Atmosphere Above Sunspot Regions
Authors: Brynildsen, N.; Brekke, P.; Haugan, S. V. H.; Kjeldseth-Moe,
O.; Maltby, P.; Wikstøl, Ø.
Bibcode: 2000AdSpR..25.1743B
Altcode:
Based on simultaneous observations of 10 EUV emission lines with the
Coronal Diagnostic Spectrometer - CDS on the Solar and Heliospheric
Observatory - SOHO we study the spatial distributions of both line
emission and line-of-sight velocity in the atmosphere above 17
sunspots. We find that both the enhanced EUV line emissions and the
velocities are distributed non-uniformly over the sunspot regions. Areas
with enhanced line emission tend to be red shifted, but they seldom
coincide exactly with areas with enhanced velocity. Bright sunspot
plumes with motion directed away from the observer are observed in
most of the sunspot regions
Title: EUV Observations of Sunspot Regions with CDS on SOHO
Authors: Brynildsen, N.; Brekke, P.; Haugan, S. V. H.; Kjeldseth-Moe,
O.; Maltby, P.
Bibcode: 1999ASPC..184..266B
Altcode:
The spatial distributions of line emission and line-of-sight velocity in
seventeen different sunspot regions are studied, based on observations
with the Coronal Diagnostic Spectrometer - CDS on SOHO. Ten EUV emission
lines, formed in the chromosphere, transition region, and corona are
observed. Enhanced EUV line emissions in the transition region are
distributed non-uniformly over the active regions and are located both
inside and outside sunspots. Most sunspot regions show strongly enhanced
transition region line emission above the spot, i.e. sunspot plumes
are reinvented. From wavelength shifts we derive the line-of-sight
velocity, relative to the average velocity in the rastered area, 120"
x 120". In sunspot plumes we find that the motion is directed away from
the observer and increases with increasing line formation temperature,
T, reaches a maximum up to 40 km s-1 close to log T ≅ 5.5,
then decreases abruptly. The spatial extent of both emission features
and flow regions increase with increasing temperature within the
transition region. The observations show a marked difference between
the transition region and the low corona, both regarding the spatial
distributions of line emission and line-of-sight velocity.
Title: A Transition Region Eruption Observed with CDS, TRACE and EIT
Authors: Brekke, P.; Kjeldseth-Moe, O.; Fredvik, T.; Haugan, S. V. H.;
Tarbell, T. D.; Gurman, J. B.
Bibcode: 1999AAS...194.5905B
Altcode: 1999BAAS...31..918B
An ejection of plasma on the west limb has been observed with CDS,
TRACE and EIT on 19 May 1998. The start of the eruption coincided
with a weak flare observed with GOES. Erupting material rose to 120
Mm above the solar surface in 17 min, and then fell back to the solar
surface. Vertical velocities of 200 km s(-1) are estimated from a series
of TRACE images in the C(+3) resonance lines at 155 nm and from EIT
images in the 19.5 nm band, while Doppler shifts of the transition
region lines observed with CDS yield maximum horizontal velocities
of 300 km s(-1) at the top of the plasma trajectories. The similar
appearance and time variation of the eruption as seen with all three
instruments indicate the presence of a multi-temperature plasma in
spatial regions less than 1-2 arc seconds, with temperatures ranging
from 10(5) K to 1.5 MK. The material did not have the momentum to break
loose from the Sun and was not associated with any CME observed with
LASCO. However, we may speculate that CMEs are similar to the eruption
observed, with even higher speeds involved.
Title: Time Variation of Active Region Loops Observed with CDS on SOHO
Authors: Fredvik, T.; Kjeldseth-Moe, O.; Brekke, P.; Haugan, S. V. H.
Bibcode: 1999AAS...194.5904F
Altcode: 1999BAAS...31R.918F
The emission from plasma filled loops, 10(4) K < T <1.5 MK,
above active regions are much more time variable than previously
considered. These loops, which define the solar atmosphere above active
regions in this temperature range, appear or disappear, the emission
along their length change, or they change shape or expand outward,
all on time scales of 10-20 minutes. In this paper we report on an
investigation with CDS on SOHO of 20 loop systems observed on the solar
limb between September 1997 and May 1998. We describe the apparent
isothermal appearance of many loops and discuss to what extent loops
radiating in different emission lines, i.e. at different temperatures,
are co-located within their recorded widths. Finally, we demonstrate
the time variability of loop systems at different temperatures, and
show how the rapidly changing conditions require a new conception of
loop systems that has never before been seriously considered.
Title: SOHO Observations of the Structure and Dynamics of Sunspot
Region Atmospheres
Authors: Brynildsen, N.; Maltby, P.; Brekke, P.; Haugan, S. V. H.;
Kjeldseth-Moe, O.
Bibcode: 1999SoPh..186..141B
Altcode:
We present results from a study of the spatial distributions of line
emission and relative line-of-sight velocity in the atmosphere above
17 sunspot regions, from the chromosphere, through the transition
region and into the corona, based on simultaneous observations of ten
EUV emission lines with the Coronal Diagnostic Spectrometer - CDS on
SOHO. We find that the spatial distributions are nonuniform over the
sunspot region and introduce the notation 'sunspot loop' to describe an
enhanced transition region emission feature that looks like a magnetic
loop, extending from inside the sunspot to the surrounding regions. We
find little evidence for the siphon flow. Attention is given to the time
variations since we observe both a rapid variation with a characteristic
time of a few to several minutes and a slow variation with a time
constant of several hours to ≈ 1 day. The most prominent features
in the transition region intensity maps are the sunspot plumes. We
introduce an updated criterion for the presence of plumes and find
that 15 out of 17 sunspots contain a plume in the temperature range
logT≈5.2-5.6. The relative line-of-sight velocity in sunspot plumes
is high and directed into the Sun in the transition region. Almost
all the sunspot regions contain one or a few prominent, strongly
redshifted velocity channels, several of the channels extend from the
sunspot plume to considerable distances from the sunspot. The flow
appears to be maintained by plasmas at transition region temperatures,
moving from regions located at a greater height outside the sunspots
and towards the sunspot. The spatial correlation is high to moderate
between emission lines formed in the transition region lines, but
low between the transition region lines and the coronal lines. From
detailed comparisons of intensity and velocity maps we find transition
region emission features without any sign of coronal emission in the
vicinity. A possible explanation is that the emission originates in
magnetic flux tubes that are too cold to emit coronal emission. The
comparisons suggest that gas at transition region temperature occur in
loops different from loops with coronal temperature. However, we cannot
exclude the presence of transition region temperatures close to the
footpoints of flux tubes emitting at coronal temperatures. Regions with
enhanced transition region line emission tend to be redshifted, but the
correlation between line emission and relative line-of-sight velocity
is weak. We extend our conditional probability studies and confirm
that there is a tendency for line profiles with large intensities and
red shifts (blue shifts) above the average to constitute an increasing
(decreasing) fraction of the profiles as the wavelength shift increases.
Title: Anomalous Line Shifts From Local Intensity Gradients on the
Soho/cds NIS Detector
Authors: Haugan, S. V. H.
Bibcode: 1999SoPh..185..275H
Altcode:
Line shifts for some emission lines on the SOHO/CDS NIS detector
appear to be strongly correlated with local intensity gradients along
the slit in a way that seems impossible to explain with a physical
solar model. Line widths also show a correlation with local intensity
gradients. The most plausible instrumental explanation seems to be an
elliptical, tilted point-spread function inducing the line shifts. A
toy model demonstrating the essentials of the observed behaviour is
presented. The effective point-spread function of the instrument appears
to modify the line shape into something other than a Gaussian, leaving
highly structured residuals after line fitting, including 'ghost' images
in some pixel planes. The cause of these effects is yet unknown, but
they should warrant experiments on the engineering model to reproduce
the observed effects, shedding light on the nature of the aberrations.
Title: Systematic errors in one-dimensional light-curve convolution
for extended sources
Authors: Haugan, S. V. H.
Bibcode: 1999MNRAS.303..471H
Altcode:
One-dimensional contour-following methods have proved an effective
means of studying the statistics of microlensing light curves for point
sources. For extended sources, however, convolving a point source light
curve with a one-dimensional source profile results in systematic
deviations from the true light curve. This paper demonstrates that
these effects are generic (regardless of source size), and attempts
to quantify the effects so that proper caution may be taken when
interpreting previous results.
Title: Flows in Sunspot Plumes Detected with SOHO
Authors: Brynildsen, N.; Maltby, P.; Brekke, P.; Fredvik, T.; Haugan,
S. V. H.; Kjeldseth-Moe, O.; Wikstol, O.
Bibcode: 1998ApJ...504L.135B
Altcode: 1998astro.ph..5249B
In the Letter, ``Flows in Sunspot Plumes Detected with the Solar and
Heliospheric Observatory'' by N. Brynildsen, P. Maltby, P. Brekke,
T. Fredvik, S. V. H. Haugan, O. Kjeldseth-Moe, and Ø. Wikstøl (ApJ,
502, L85 [1998]), the following correction should be made: In
the last line on page L86, which reads ``peak line intensity I>=5
are located (1) above the umbra or, '' an ``Ī'' should be inserted so
that the revised line reads ``peak line intensity I>=5Ī are located
(1) above the umbra or.''
Title: Flows in Sunspot Plumes Detected with the Solar and
Heliospheric Observatory
Authors: Brynildsen, N.; Maltby, P.; Brekke, P.; Fredvik, T.; Haugan,
S. V. H.; Kjeldseth-Moe, O.; Wikstøl, Ø.
Bibcode: 1998ApJ...502L..85B
Altcode:
Bright extreme-UV sunspot plumes have been observed in eight out of
11 different sunspot regions with the Coronal Diagnostic Spectrometer
on Solar and Heliospheric Observatory. From wavelength shifts, we
derive the line-of-sight velocity relative to the average velocity
in the rastered area, 120''×120''. In sunspot
plumes, we find that the motion is directed away from the observer
and increases with increasing line formation temperature, reaches a
maximum between 15 and 41 km s-1 close to log logT~5.5,
then decreases abruptly. The flow field in the corona is not well
correlated with the flow in the transition region, and we discuss
briefly the implication of this finding.
Title: SOHO Observations of the Connection Between Line Profile
Parameters in Active and Quiet Regions and the Net Red Shift in EUV
Emission Lines
Authors: Brynildsen, N.; Brekke, P.; Fredvik, T.; Haugan, S. V. H.;
Kjeldseth-Moe, O.; Maltby, P.; Harrison, R. A.; Wilhelm, K.
Bibcode: 1998SoPh..181...23B
Altcode:
We present high spatial and spectral resolution observations of
one active and one quiet-Sun region, obtained with CDS and SUMER on
SOHO. The connections between the line profile parameters are studied
and a systematic wavelength shift towards the red with increasing peak
line intensity (line broadening) is detected. The large scatter in
the data calls for another approach. We apply conditional probability
analysis to a series of EUV emission lines and find significant
correlations between line profile parameters. For a given interval in
wavelength shift we find that: (1) line profiles with large intensities
(line widths) and red shifts above the average constitute an increasing
fraction of the profiles as the relative wavelength shift increases,
(2) line profiles with large intensities (line widths) and blue
shifts compared to the average, on the other hand, constitute a
decreasing fraction of the profiles as the relative wavelength shift
increases. These results extend the findings of an earlier quiet-Sun
study from one to several emission lines and expand the validity to
include the active region. Interestingly, the active region observations
show correlations between peak line intensity and wavelength shift in
the coronal lines.
Title: EUV Spectroscopy of the Sunspot Region NOAA 7981 Using SOHO -
II. Velocities and Line Profiles
Authors: Brynildsen, N.; Brekke, P.; Fredvik, T.; Haugan, S. V. H.;
Kjeldseth-Moe, O.; Maltby, P.; Harrison, R. A.; Pike, C. D.; Rimmele,
T.; Thompson, W. T.; Wilhelm, K.
Bibcode: 1998SoPh..179..279B
Altcode:
We have studied the dynamics in the sunspot transition region between
the chromosphere and the corona and investigated the extension of
the flow field into the corona. Based on EUV spectra of a medium size
sunspot and its surroundings, NOAA 7981, observed with CDS and SUMER
on SOHO, we derive line-of-sight velocities and study the line profiles
for a series of emission lines.
Title: Extreme-Ultraviolet Sunspot Plumes Observed with SOHO
Authors: Maltby, P.; Brynildsen, N.; Brekke, P.; Haugan, S. V. H.;
Kjeldseth-Moe, O.; Wikstøl, Ø.; Rimmele, T.
Bibcode: 1998ApJ...496L.117M
Altcode: 1998astro.ph..1144M
Bright EUV sunspot plumes have been observed in five out of nine sunspot
regions with the Coronal Diagnostic Spectrometer on the Solar and
Heliospheric Observatory. In the other four regions, the brightest line
emissions may appear inside the sunspot but are mainly concentrated in
small regions outside the sunspot areas. These results are in contrast
to those obtained during the Solar Maximum Mission but are compatible
with the Skylab mission results. The present observations show that
sunspot plumes are formed in the upper part of the transition region,
occur in both magnetic unipolar and bipolar regions, and may extend
from the umbra into the penumbra.
Title: EUV Spectroscopy of the Sunspot Region NOAA 7981 Using SOHO -
I. Line Emission and Time Dependence
Authors: Brynildsen, N.; Brekke, P.; Fredvik, T.; Haugan, S. V. H.;
Kjeldseth-Moe, O.; Maltby, P.; Harrison, R. A.; Pike, C. D.; Rimmele,
T.; Thompson, W. T.; Wilhelm, K.
Bibcode: 1998SoPh..179...43B
Altcode:
EUV spectra of a medium-size sunspot and its surroundings, NOAA 7981,
were obtained on 2 August 1996 with the Coronal Diagnostic Spectrometer
(CDS) and the Solar Ultraviolet Measurements of Emitted Radiation
(SUMER) on the Solar and Heliospheric Observatory (SOHO). The spectral
lines formed in the transition region and corona show considerable
structure and large deviations from a uniform spatial distribution over
the active region. Enhanced EUV emissions in transition region lines
are concentrated in small regions outside the umbra of the sunspot
throughout most of the observing sequence. Only during a short,
active period do we find an enhanced line emission that reaches into
the umbra. Preliminary values for the umbral intensity are given.
Title: Three Dimensional EUV Imaging of Sunspot Regions Observed
with SOHO
Authors: Brynildsen, N.; Brekke, P.; Haugan, S. V. H.; Kjeldseth-Moe,
O.; Maltby, P.; Harrison, R. A.; Rimmele, T.; Wilhelm, K.
Bibcode: 1998ASPC..155..171B
Altcode: 1998sasp.conf..171B
No abstract at ADS
Title: Inconstancy of the Transition Region - Variable and Dynamic
Active Region Loops
Authors: Kjeldseth-Moe, O.; Brekke, P.; Haugan, S. V. H.
Bibcode: 1998ESASP.417..153K
Altcode: 1998cesh.conf..153K
No abstract at ADS
Title: The Non-Uniformity in the Sunspot Transition Region
Authors: Brynildsen, N.; Brekke, P.; Fredvik, T.; Haugan, S. V. H.;
Kjeldseth-Moe, O.; Maltby, P.; Harrison, R. A.; Rimmele, T.;
Wilhelm, K.
Bibcode: 1997ESASP.404..257B
Altcode: 1997cswn.conf..257B
No abstract at ADS
Title: Transition Region Velocities and Line Profiles in the Sunspot
Region 7981
Authors: Brynildsen, N.; Brekke, P.; Fredvik, T.; Haugan, S. V. H.;
Kjeldseth-Moe, O.; Maltby, P.; Harrison, R. A.; Pike, C. D.; Rimmele,
T. Thompson, W. T.; Wilhelm, K.
Bibcode: 1997ESASP.404..251B
Altcode: 1997cswn.conf..251B
No abstract at ADS
Title: The Net Redshifts in EUV Emission Lines and the Connection
Between Intensity and Doppler Shift
Authors: Brynildsen, N.; Fredvik, T.; Maltby, P.; Kjeldseth-Moe, O.;
Brekke, P.; Haugan, S. V. H.; Harrison, R. A.; Wilhelm, K.
Bibcode: 1997ESASP.404..263B
Altcode: 1997cswn.conf..263B
No abstract at ADS
Title: EUV Line Emission and Time Dependence in the Sunspot Region
NOAA 7981
Authors: Brynildsen, N.; Brekke, P.; Fredvik, T.; Haugan, S. V. H.;
Kjeldseth-Moe, O.; Maltby, P.; Harrison, R. A.; Pike, C. D.; Rimmele,
T.; Thompson, W. T.; Wilhelm, K.
Bibcode: 1997ESASP.404..245B
Altcode: 1997cswn.conf..245B
No abstract at ADS
Title: Flows and Dynamics in the Corona Observed with the Coronal
Diagnostic Spectrometer (cds)
Authors: Brekke, P.; Kjeldseth-Moe, O.; Brynildsen, N.; Maltby, P.;
Haugan, S. V. H.; Harrison, R. A.; Thompson, W. T.; Pike, C. D.
Bibcode: 1997SoPh..170..163B
Altcode:
EUV spectra obtained with the Coronal Diagnostic Spectrometer (CDS)
on the Solar and Heliospheric Observatory (SOHO) show significant flows
of plasma in active region loops, both at coronal and transition region
temperatures. Wavelength shifts in the coronal lines Mgix 368 Å and
Mgx 624 Å corresponding to upflows in the plasma reaching velocities
of 50 km s-1 have been observed in an active region. Smaller
velocities are detected in the coronal lines Fexvi 360 Å and Sixii
520 Å. Flows reaching 100 km s-1 are observed in spectral
lines formed at transition region temperatures, i.e., Ov 629 Å and
Oiii 599 Å, demonstrating that both the transition region and the
corona are clearly dynamic in nature. Some high velocity events show
even higher velocities with line profiles corresponding to a velocity
dispersion of 300-400 km s-1. Even in the quiet Sun there
are velocity fluctuations of 20 km s-1 in transition region
lines. Velocities of the magnitude presented in this paper have never
previously been observed in coronal lines except in explosive events
and flares. Thus, the preliminary results from the CDS spectrometer
promise to put constraints on existing models of the flows and energy
balance in the solar atmosphere. The present results are compared to
previous attempts to observe flows in the corona.
Title: Simulation of Microlensing Lightcurves by Combining Contouring
and Rayshooting
Authors: Haugan, S. V. H.
Bibcode: 1996IAUS..173..275H
Altcode: 1995astro.ph..8109H
The contouring methods described by Lewis et al. (1993) and Witt (1993)
are very efficient and elegant for obtaining the magnification of a
point source moving along a straight track in the source plane. The
method is, however, not very efficient for extended sources, because the
amplification needs to be computed for numerous parallel tracks and then
convolved with the source profile. Rayshooting is an efficient algorithm
for relatively large sources, but the computing time increases with the
inverse of the source area for a given noise level. This poster presents
a hybrid method, using the contouring method in order to find only those
parts of the lens area that contribute to the light curve through the
rayshooting. Calculations show that this method has the potential to
be $10$--$10^5$ times more efficient than crude rayshooting techniques.
Title: Separating Intrinsic and Microlensing Variability Using
Parallax Measurements
Authors: Haugan, S. V. H.
Bibcode: 1996IAUS..173..277H
Altcode: 1995astro.ph..8112H
In gravitational lens systems with 3 or more resolved images of
a quasar, the intrinsic variability may be unambiguously separated
from the microlensing variability through parallax measurements from 3
observers when there is no relative motion of the lens masses (Refsdal
1993). In systems with fewer than 3 resolved images, however, this
separation is not straightforward. A general approach that may be used
for this purpose is presented. For simplicity, only the one-dimensional
case is considered in detail: Given a well-sampled time series of
the observed flux at two points in space with a known separation,
choosing a velocity $v_{\perp}$ of the observers perpendicular to
the line of sight determines the microlensing magnification history,
and thereby also the intrinsic variability. The velocity is chosen
by minimizing some measure ($\chi^2$) of the residual intrinsic
variability. In many cases this gives a close approximation to the
true magnification. In cases where the relative motion of the lensing
point masses is important, only a partial separation will be possible.
Title: The Microlensing Events In Q2237+0305A: No Case Against Small
Masses/Large Sources
Authors: Haugan, S. V. H.
Bibcode: 1996IAUS..173..255H
Altcode: 1995astro.ph..8103H
It is demonstrated that the 1988-90 microlensing events in image A
of Q2237+0305 reported by Racine (1992) do not exclude microlensing
models with very low average mass, making the source radius larger
than the projected Einstein radius $\eta_0$ (Refsdal and Stabell 1991,
1993). This is contrary to what has been claimed by Witt and Mao
(1994). Since these events are the best resolved microlensing events
recorded in Q2237+0305, further work should not exclude the possibility
of a large source when interpreting lightcurve data.
Title: CDS quicklook display software
Authors: Brekke, P.; Haugan, S. V. H.; Brynildsen, Nils
Bibcode: 1994ESASP.373..437B
Altcode: 1994soho....3..437B
No abstract at ADS
Title: Correlation analysis of microlensing lightcurves
Authors: Haugan, S. V.; Refsdal, S.; Stabell, R.
Bibcode: 1993LIACo..31..447H
Altcode: 1993glu..conf..447H
No abstract at ADS