J/A+A/691/A308 Physical properties of DESI galaxies (Siudek+, 2024)
Value added catalog of physical properties of more than 1.3 million galaxies
from the DESI survey.
Skiudek M., Pucha R., Mezcua M., Juneau S., Aguilar J., Ahlen S., Brooks D.,
Circosta C., Claybaugh T., Cole S., Dawson K., de la Macorra A., Dey A.,
Dey B. Doel P., Font-Ribera A., Forero-Romero J.E., Gaztanaga E.,
Gontcho A Gontcho S., Gutierrez G., Honscheid K., Howlett C., Ishak M.,
Kehoe R., Kirkby D., Kisner T., Kremin A., Lambert A., Landriau M.,
Le Guillou L., Manera M., Martini P., Meisner A., Miquel R., Moustakas J.,
Newman J.A., Niz G., Pan Z., Percival W.J., Poppett C., Prada F., Rossi G.,
Saintonge A., Sanchez E., Schlegel D., Scholte D., Schubnell M., Seo H.,
Speranza F., Sprayberry D., Tarle G., Weaver B.A., Zou H.
<Astron. Astrophys. 691, A308 (2024)>
=2024A&A...691A.308S 2024A&A...691A.308S (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Galaxy catalogs ; Photometry, SDSS ;
Photometry, infrared
Keywords: catalogs - galaxies: active - galaxies: evolution -
galaxies: general - galaxies: nuclei - galaxies: Seyfert
Abstract:
We present an extensive catalog of the physical properties of more
than a million galaxies within the Dark Energy Spectroscopic
Instrument (DESI), one of the largest spectroscopic surveys to date.
Spanning over a full variety of target types, including emission line
galaxies and luminous red galaxies as well as quasars, our survey
encompasses an unprecedented range of spectroscopic redshifts,
stretching from 0 to 6. The physical properties, such as stellar
masses and star formation rates, are derived via the CIGALE spectral
energy distribution (SED) fitting code accounting for the contribution
coming from active galactic nuclei (AGN). Based on the modeling of the
optical-mid-infrared (grz complemented by WISE photometry) SEDs, we
study galaxy properties with respect to their location on the main
sequence. We revise the dependence of stellar mass estimates on model
choices and availability of the WISE photometry. The WISE information
is mandatory to minimize the misclassification of star-forming
galaxies as AGN. The lack of WISE bands in SED fits leads to elevated
AGN fractions for 68% of star-forming galaxies identified using
emission line diagnostic diagram but does not affect significantly
their stellar mass nor star formation estimates.
Description:
This value-added catalog contains physical properties of DESI EDR
galaxies derived with CIGALE (v.22.1; Boquien et al.
2019A&A...622A.103B 2019A&A...622A.103B, Cat. J/A+A/622/A103) accounting for AGN
contribution. To generate the grid of models we use a delayed star
formation history (SFH) model with an optional exponential burst and
Bruzal & Charlot (2003MNRAS.344.1000B 2003MNRAS.344.1000B) single stellar population
models assuming Chabrier (2003ApJ...586L.133C 2003ApJ...586L.133C) initial mass function
and solar metallicity. We also include the standard nebular emission
model from Inoue et al. ( 2011MNRAS.418.2527I 2011MNRAS.418.2527I ) and model dust
attenuation using Calzetti et al. (2000ApJ...533..682C 2000ApJ...533..682C) attenuation
curve. The reprocessed dust emission is modeled adopting the dust
emission models of Dale et al. (2014ApJ...784...83D 2014ApJ...784...83D). The AGN emission
is modeled using the models from Fritz et al. (2006MNRAS.366..767F 2006MNRAS.366..767F) .
CIGALE simultaneously fits the AGN and galaxy component using all the
available photometry (g, r, z, W1, W2, W3 and W4) and returns
estimates of the main galaxy properties such as stellar mass, star
formation rate, and the relative contribution of the dusty torus of
the AGN to the total IR luminosity - the AGN fraction using a
Bayesian-like analysis. We note that incorporating AGN models does not
exclude a scenario where the galaxy does not host an AGN (or its
emission is negligible). In such cases, the AGN fraction is close to 0
(AGNfrac<0.1). The quality of the fit is expressed by the reduced
chi2, the estimates and errors of physical properties are the
likelihood-weighted means and standard deviations of the probability
distribution function, respectively (Boquien et al.,
2019A&A...622A.103B 2019A&A...622A.103B, Cat. J/A+A/622/A103). The cosmology assumed is
WMAP7.
The catalog accounts for 1,286,124 of DESI EDR galaxies.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 766 1337250 Catalog
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See also:
VII/292 : DESI Legacy Imaging Surveys DR8 photometric redshifts (Duncan, 2022)
https://data.desi.lbl.gov/doc : DESI Home Page
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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1- 19 I19 --- Target Unique DESI Target ID (TARGETID)
21- 27 A7 --- Survey Survey name (SURVEY)
29- 34 A6 --- Program Program name (PROGRAM)
36- 40 I5 --- HEALPIX Healpix number (HEALPIX)
42- 47 A6 --- SpType Redrock spectral classification
(SPECTYPE)
49- 63 F15.11 deg RAdeg Right ascension (J2000) from target
catalog (RA)
65- 79 F15.11 deg DEdeg Declination (J2000) from target
catalog (DEC)
81- 84 I4 --- Release Legacy Surveys (LS) Release (RELEASE)
86- 96 F11.8 --- z Redshift (Z)
98-104 F7.3 --- chi2 ?=-99 Reduced chi2 defining the quality
of the fit: for a more reliable
estimations the cut of chi2≲15 is
recommended (CHI2)
106-113 F8.4 [Msun] logM ?=-99 logarithm of the stellar mass
(LOGM)
115-123 F9.5 [Msun] e_logM ?=-99 Error on logarithm of the
stellar mass (LOGM_ERR)
125-133 F9.5 [Msun/yr] logSFR ?=-99 logarithm of the star formation
rate averaged over 10Myr (LOGSFR)
135-144 F10.6 [Msun/yr] e_logSFR ?=-99 Error on logarithm of star
formation rate averaged over 10Myr
(LOGSFR_ERR)
146-157 E12.6 W AGNLum Total Luminosity of the AGN (AGNLUM)
159-166 F8.4 --- AGNFrac ?=-99 Fraction of the total IR emission
coming from the AGN (AGNFRAC) (1)
168-175 F8.4 deg AGNPsy ?=-99 Viewing angle, with ∼30deg and
∼70deg, for type 1 and type 2 AGN,
respectively (AGNPSY)
177-188 E12.6 W/Hz Lnu-u Rest-frame luminosity in u band
(LNU_U) (2)
190-201 E12.6 W/Hz Lnu-g Rest-frame luminosity in g band
(LNU_G) (2)
203-214 E12.6 W/Hz Lnu-r Rest-frame luminosity in r band
(LNU_R) (2)
216-227 E12.6 W/Hz Lnu-i Rest-frame luminosity in i band
(LNU_I) (2)
229-240 E12.6 W/Hz Lnu-z Rest-frame luminosity in z band
(LNU_Z) (2)
242-250 F9.5 mag NUV-r ?=-99 Rest-frame NUV-r color (AB)
(NUVR)
252-260 F9.5 mag r-K ?=-99 Rest-frame r-K color (AB) (RK)
262-270 F9.5 mag U-V ?=-99 Rest-frame U-V color (AB) (UV)
272-280 F9.5 mag V-J ?=-99 Rest-frame V-J color (AB) (VJ)
282-290 F9.5 mag g-r ?=-99 Rest-frame g-r color (AB) (GR)
292-303 E12.6 W/Hz e_Lnu-u ?=-99 Error of the rest-frame
luminosity in a given band (LNUUERR)
305-316 E12.6 W/Hz e_Lnu-g ?=-99 Error of the rest-frame
luminosity in g band (LNUGERR)
318-329 E12.6 W/Hz e_Lnu-r ?=-99 Error of the rest-frame
luminosity in r band (LNURERR)
331-342 E12.6 W/Hz e_Lnu-i ?=-99 Error of the rest-frame
luminosity in i band (LNUIERR)
344-355 E12.6 W/Hz e_Lnu-z ?=-99 Error of the rest-frame
luminosity in z band (LNUZERR)
357-366 F10.6 mag e_NUV-r ?=-99 Error of the rest-framed color
NUV-r (NUVR_ERR)
368-377 F10.6 mag e_r-K ?=-99 Error of the rest-framed color
r-K (RK_ERR)
379-388 F10.6 mag e_U-V ?=-99 Error of the rest-framed color
U-V (UV_ERR)
390-399 F10.6 mag e_V-J ?=-99 Error of the rest-framed color
V-J (VJ_ERR)
401-410 F10.6 mag e_g-r ?=-99 Error of the rest-framed color
g-r (GR_ERR)
412-423 E12.6 --- Flag-MassPDF Flag expressed by Mbest/Mbayes to
reject stellar mass estimates with
broad PDF and/or complex likelihood
distribution (FLAG_MASSPDF) (3)
425-436 E12.6 --- Flag-SFRPDF Flag expressed by SFRbest/SFRbayes to
reject SFR estimates with broad PDF
and/or complex likelihood distribution
(FLAG_SFRPDF) (4)
438 I1 --- Flag-Opt Flag to preselect sources observed with
high signal-to-noise (S/N≥10 in
optical bands(g, r, z)
(FLAGOPTICAL) (5)
440 I1 --- Flag-IR Flag to preselect sources observed with
high signal-to-noise (S/N≥3 in
WISE bands(W1, W2, W3, W4)
(FLAGINFRARED) (6)
442-453 F12.6 3.63uJy Fluxg Flux in g band in nanomaggy
(FLUX_G) (7)
455-467 F13.6 3.63uJy Fluxr Flux in r band in nanomaggy
(FLUX_R) (7)
469-481 F13.6 3.63uJy Fluxz Flux in z band in nanomaggy
(FLUX_Z) (7)
483-495 F13.6 3.63uJy FluxW1 Flux in W1 band in nanomaggy
(FLUX_W1) (7)
497-509 F13.6 3.63uJy FluxW2 Flux in W2 band in nanomaggy
(FLUX_W2) (7)
511-523 F13.6 3.63uJy FluxW3 Flux in W3 band in nanomaggy
(FLUX_W3) (7)
525-539 F15.6 3.63uJy FluxW4 Flux in W4 band in nanomaggy
(FLUX_W4) (7)
541-551 F11.6 3.63uJy-2 Flux-ivarg Inverse variance of the flux in g band
in nanomaggy-2 (FLUXIVARG)
553-563 F11.6 3.63uJy-2 Flux-ivarr Inverse variance of the flux in r band
in nanomaggy-2 (FLUX_IVAR/R)
565-574 F10.6 3.63uJy-2 Flux-ivarz Inverse variance of the flux in z band
in nanomaggy-2 (FLUXIVARZ)
576-584 F9.6 3.63uJy-2 Flux-ivarW1 Inverse variance of the flux in W1 band
in nanomaggy-2 (FLUXIVARW1)
586-594 F9.6 3.63uJy-2 Flux-ivarW2 Inverse variance of the flux in W2 band
in nanomaggy-2 (FLUXIVARW2)
596-603 F8.6 3.63uJy-2 Flux-ivarW3 Inverse variance of the flux in W3 band
in nanomaggy-2 (FLUXIVARW3)
605-612 F8.6 3.63uJy-2 Flux-ivarW4 Inverse variance of the flux in W4 band
in nanomaggy-2 (FLUXIVARW4)
614-621 F8.6 --- MWTransg [0/1] Milky Way foreground dust
transmission factor in g band
(MWTRANSMISSIONG)
623-630 F8.6 --- MWTransr [0/1] Milky Way foreground dust
transmission factor in r band
(MWTRANSMISSIONR)
632-639 F8.6 --- MWTransz [0/1] Milky Way foreground dust
transmission factor in z band
(MWTRANSMISSIONZ)
641-648 F8.6 --- MWTransW1 [0/1] Milky Way foreground dust
transmission factor in W1 band
(MWTRANSMISSIONW1)
650-657 F8.6 --- MWTransW2 [0/1] Milky Way foreground dust
transmission factor in W2 band
(MWTRANSMISSIONW2)
659-666 F8.6 --- MWTransW3 [0/1] Milky Way foreground dust
transmission factor in W3 band
(MWTRANSMISSIONW3)
668-675 F8.6 --- MWTransW4 [0/1] Milky Way foreground dust
transmission factor in W3 band
(MWTRANSMISSIONW4)
677-688 E12.6 --- SNR-g Signal-to-noise in g band calculated
as FLUX*sqrt(FLUX_IVAR) (SNR_G)
690-701 E12.6 --- SNR-r Signal-to-noise in r band calculated
as FLUX*sqrt(FLUX_IVAR) (SNR_R)
703-714 E12.6 --- SNR-z Signal-to-noise in z band calculated
as FLUX*sqrt(FLUX_IVAR) (SNR_Z)
716-727 E12.6 --- SNR-W1 Signal-to-noise in W1 band calculated
as FLUX*sqrt(FLUX_IVAR) (SNR_W1)
729-740 E12.6 --- SNR-W2 Signal-to-noise in W2 band calculated
as FLUX*sqrt(FLUX_IVAR) (SNR_W2)
742-753 E12.6 --- SNR-W3 Signal-to-noise in W3 band calculated
as FLUX*sqrt(FLUX_IVAR) (SNR_W3)
755-766 E12.6 --- SNR-W4 Signal-to-noise in W4 band calculated
as FLUX*sqrt(FLUX_IVAR) (SNR_W4)
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Note (1): where 0 means no AGN contribution and 1 means 100% AGN contribution.
Note (2): rest-frame magnitudes can by derived using eq. -2.5xlog10(Lnu)+34.1.
Note (3): e.g. to clean the sample the recommended flag is 1/5≲Mbest/Mbayes≲5
Note (4): e.g. to clean the sample the recommended flag is
1/5≲SFRbest/SFRbayes≲5
Note (5): FlagOpt = 3(2/1/0) : source is observed in 3(2/1/0) band(s)
with S/N≥10
Note (6): FlagIR = 4(3/2/1/0) : source is observed in 4(3/2/1/0) band(s)
with S/N≥3
Note (7): For the reddening corrected flux use the eq.
DERED_FLUX = FLUXBAND/MWTRANSMISSION_BAND; for magnitude follow eq.
MAG_BAND = -2.5xlog10(DERED_FLUX) + 22.5.
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Acknowledgements:
Malgorzata Siudek, siudek(at)ice.csic.es
(End) Patricia Vannier [CDS] 11-Oct-2024