2022A&A...657A..90E

Query : 2022A&A...657A..90E

2022A&A...657A..90E - Astronomy and Astrophysics, volume 657A, 90-90 (2022/1-1)

Euclid preparation. XIII. Forecasts for galaxy morphology with the Euclid Survey using deep generative models.

EUCLID COLLABORATION, BRETONNIERE 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., KUMMEL 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-CRESPI 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-ANTOLINEZ 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., SANCHEZ A.G., SAPONE D., SCHIRMER M., SCHULTHEIS M., SCOTTEZ V., SEFUSATTI E., TEYSSIER R., TUTUSAUS I., VALIVIITA J., VIEL M., WHITTAKER L. and KNAPEN J.H.

Abstract (from CDS):

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 Sersic 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/arcsec2, and the Euclid Deep Survey (EDS) down to 24.9 mag/arcsec2. 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.

Abstract Copyright: © Euclid Collaboration 2022

Journal keyword(s): techniques: image processing - surveys - galaxies: structure - galaxies: evolution - cosmology: observations

Simbad objects: 1

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Number of rows : 1
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 NAME COSMOS Field reg 10 00 28.60 +02 12 21.0           ~ 2972 0

Query : 2022A&A...657A..90E

Basic data :
NAME COSMOS Field -- Region defined in the Sky
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(Ref) Object type as listed in the reference "Ref"
(acronym) Object type linked to the acronym according to the original reference
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Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
  • ra dec : right ascension and declination (unit and frame defined according to your Output Options)
    Grey values are increasing the original precision due to the computation of frame transformations
  • (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
  • [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
    position angle (in degrees North celestial pole to East)
  • quality : flag of quality
    • E ≥ 10"
    • D : 1-10" (and some old data)
    • C : 0.1-1"
    • B : 0.01-0.1" + 2MASS, Tyc
    • A : VLBI, Hipparcos
  • bibcode : bibcode of the coordinates reference
ICRS coord. (ep=J2000) : 		10 00 28.60 +02 12 21.0 [ ] D 2007ApJS..172..523M
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
  • ra dec : right ascension and declination (unit and frame defined according to your Output Options)
    Grey values are increasing the original precision due to the computation of frame transformations
  • (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
  • [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
    position angle (in degrees North celestial pole to East)
  • quality : flag of quality
    • E ≥ 10"
    • D : 1-10" (and some old data)
    • C : 0.1-1"
    • B : 0.01-0.1" + 2MASS, Tyc
    • A : VLBI, Hipparcos
  • bibcode : bibcode of the coordinates reference
FK4 coord. (ep=B1950 eq=1950) : 		09 57 53.49 +02 26 47.1 [ ]
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
  • ra dec : right ascension and declination (unit and frame defined according to your Output Options)
    Grey values are increasing the original precision due to the computation of frame transformations
  • (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
  • [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
    position angle (in degrees North celestial pole to East)
  • quality : flag of quality
    • E ≥ 10"
    • D : 1-10" (and some old data)
    • C : 0.1-1"
    • B : 0.01-0.1" + 2MASS, Tyc
    • A : VLBI, Hipparcos
  • bibcode : bibcode of the coordinates reference
Gal coord. (ep=J2000) : 		236.82224 +42.12163 [ ]
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', {sourceSize:12, color:'#30a090'})); aladin.on('objectClicked', function(object) { var objName=object.data.MAIN_ID; aladin.showPopup(object.ra,object.dec,'',''+ objName+''); });" title="Show Simbad objects"> Overlay Simbad points in this preview
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NAME COSMOS Field

References (2972 between 1850 and 2024) (Total 2972)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).
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