J/MNRAS/511/6160 BTFR's study of ∼10000 HyperLEDA galaxies (Kourkchi+, 2022)
Cosmicflows-4 the baryonic Tully-Fisher relation providing ∼10000 distances.
Kourkchi E., Tully R.B., Courtois H.M., Dupuy A., Guinet D.
<Mon. Not. R. Astron. Soc. 511, 6160-6178 (2022)>
=2022MNRAS.511.6160K 2022MNRAS.511.6160K (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Galaxies, group ; Galaxies, nearby ; Infrared ;
Optical ; Radio sources ; Photometry ; Spectroscopy ;
H I data ; Stars, masses ; Radial velocities ; Line Profiles ;
Positional data
Keywords: catalogues - galaxies: distances and redshifts - galaxies: evolution -
galaxies: fundamental parameters - galaxies: kinematics and dynamics -
galaxies: spiral
Abstract:
The interstellar gas in spiral galaxies can constitute a significant
fraction of the baryon mass and it has been demonstrated that the sum
of stellar and gas components correlates well with the kinematic
signature of the total mass content, the widths of H I line profiles.
The correlation of baryonic mass with H I linewidths is used here to
obtain distances for 9984 galaxies extending to ∼0.05c. The sample is
H I flux limited and a correction is required to account for an H I
selection bias. The absolute scale is established by 64 galaxies with
known distances from studies of Cepheid variables and/or the
magnitudes of stars at the tip of the red giant branch. The
calibration of the baryonic relationship results in a determination of
the Hubble constant of H0 = 75.5 ± 2.5 km/s/Mpc. The error
estimate is statistical. This material will be combined with
contributions from other methodologies in a subsequent paper where
systematic uncertainties will be investigated.
Description:
The empirical coupling between the luminosities of spiral galaxies and
their rotation rates [Tully-Fisher relation (TFR); Tully & Fisher
1977A&A....54..661T 1977A&A....54..661T] has an evident zeroth-order explanation: more
intrinsically luminous galaxies tend to be more massive and more
massive galaxies rotate faster under equilibrium conditions. Optical
or infrared light represents only the stellar component of mass, that
contributions from interstellar gas could be important, and the star
and gas together give representation of the total baryonic mass of a
galaxy. The correlation between the baryonic mass and the rotation
rate of a galaxy has become known as the baryonic Tully-Fisher
relation (BTFR). In this paper, is not to fully understand the physics
of the BTFR but just to use the empirically tight BTFR to measure
galaxy distances.
This study follows an investigation of the strictly stellar TFR at
Sloan Digital Sky Survey (SDSS) optical and Wide-field Infrared Space
Explorer (WISE) passbands (Kourkchi et al. 2020b). The galaxy samples
used then and now, the photometry, the inclinations, the reddening
assumptions, and the H I linewidths, are the same. The additional
component, neutral hydrogen fluxes, is gathered both from observations
within our collaboration and from those by others. We construct a
sample of 10153 galaxies by using BTFR formalism to compute and report
severals properties as component masses, galaxy and group radial
velocities, band widths, fluxes, optical and infrared magnitudes and
coordinates, all these data helping us to retreive precise galactic
distance values (i.e see section 4 Calculation of distances) all
presented in the table3.dat, (i.e see also sections 2 to formalism
details and section 3 for ZP calibrations).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 289 10153 Observed and inferred properties of our galaxy
sample used in this study
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See also:
J/ApJ/902/145 : Cosmicflows-4 Tully-Fisher distances (Kourkchi+, 2020)
J/A+A/646/A113 : Towards Cosmicflows-4 HI data catalog (Dupuy+, 2021)
J/AJ/138/1938 : EDD All Digital HI profile catalog (Courtois+, 2009)
J/AJ/149/171 : 2MASS galaxy group catalog (Tully, 2015)
J/ApJ/843/16 : Galaxy groups within 3500km/s (Kourkchi+, 2017)
J/MNRAS/414/2005 : Cosmic flows observations (Courtois+, 2011)
J/ApJ/676/184 : Peculiar motion away from the Local Void (Tully+, 2008)
VII/237 : HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)
VII/238 : HYPERLEDA. II. Homogenized HI data (Paturel+, 2003)
J/ApJ/861/49 : ALFALFA extragalactic HI source catalog (Haynes+, 2018)
J/ApJ/816/L14 : Tully-Fisher relation in disk galaxies from SPARC
(Lelli+, 2016)
J/ApJ/792/129 : WISE W1/W2 Tully-Fisher relation calibrator data
(Neill+, 2014)
VII/75 : Infrared Photometry and 21cm data for nearby galaxies
(Aaronson+, 1982)
J/ApJ/896/3 : Cosmicflows-4: Tully-Fisher relation calibrations
(Kourkchi+, 2020)
J/ApJ/884/82 : SDSS, WISE and HI data of local spiral galaxies
(Kourkchi+, 2019)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 7 I7 --- PGC The ID number of the galaxy in the
Principal Galaxy Catalog (PGC) (1)
9 I1 --- f_PGC [] Quality flag (Flag) (2)
11- 15 F5.2 mag DMav ? The average of distance moduli measured
using optical and infrared data (DMav)
17- 20 F4.2 mag e_DMav ? The reported DMav uncertainty is the
maximum adjusted error of the optical and
infrared moduli (errDMav)
22- 26 F5.2 mag DMriz ? The measured distance modulus from the
averaged optical BTFRi (DMriz) (3)
28- 38 F11.2 mag e_DMriz []? The DMriz statistical error on the
measured modulii (errDMriz) (4)
40- 44 F5.2 mag DMW1 ? The measured distance modulus from the
WISE NIR W1 BTFR (DMW1) (5)
46- 56 F11.2 mag e_DMW1 []? The DMW1 statistical error on the
measured moduli (errDMW1) (6)
58- 64 I7 --- PGCID The PGC ID of the dominant galaxy in the
parent group from Kourkchi & Tully
2017ApJ...843...16K 2017ApJ...843...16K, Cat. J/ApJ/843/16
(1PGC)
66- 71 I6 --- Nest ? The parent group ID in the Two Micron
All-Sky Survey 2MASS group catalogue
Tully 2015AJ....149..171T 2015AJ....149..171T,
Cat. J/AJ/149/171 (Nest)
73- 78 F6.3 [Msun] logM*riz ? The logarithm of the average stellar mass
calculated based on SDSS photometry data at
the r, i, and z bands (logM*)
80- 85 F6.3 [Msun] logM*W1 ? The logarithm of the stellar mass
calculated based on W1-band photometry
data (logM*W1) (7)
87- 92 F6.3 [Msun] logMg ? The logarithm of the galaxy gas mass
calculated using 1.33*MHI (logMg) (8)
94- 99 F6.3 [Msun] logMb ? The logarithm of the total baryonic mass
of a galaxy in stellar and gas forms
(logMb) (9)
101- 105 I5 km/s Vh Heliocentric velocity from H I observations
(Vh)
107- 111 I5 km/s VLS Radial velocity relative to the Local Sheet
from Tully et al. 2008ApJ...676..184T 2008ApJ...676..184T,
Cat. J/ApJ/676/184 (VLS)
113- 117 I5 km/s VCMB Radial velocity in the rest frame of the
cosmic microwave background (V_CMB)
119- 123 F5.3 --- f The cosmological correction factor fj
(fj) (10)
125- 129 F5.3 [km/s] logWimx The logarithm of the inclination-corrected
H I linewidth (logWimx) (11)
131- 135 F5.3 [km/s] e_logWimx Mean error of logWimx (errlogWimx)
137- 144 F8.2 Jy.km/s F21 The H I 21-cm integrated flux (F21)
146- 151 F6.2 Jy.km/s e_F21 Mean error of F21 (errF21)
153- 154 I2 deg i The inclination angle of the galaxy (Inc)
156- 163 I8 deg e_i ?=-1000000 Mean error of i (errInc)
165- 169 F5.2 mag g*mag ? The SDSS g corrected magnitude in the AB
system (g*) (12)
171- 175 F5.2 mag r*mag ? The SDSS r corrected magnitude in the AB
system (r*) (12)
177- 181 F5.2 mag i*mag ? The SDSS i corrected magnitude in the AB
system (i*) (12)
183- 187 F5.2 mag z*mag ? The SDSS z corrected magnitude in the AB
system (z*) (12)
189- 193 F5.2 mag W1*mag ? The WISE W1 corrected magnitude in the AB
system (W1*) (12)
195- 199 F5.2 mag W2*mag ? The WISE W2 corrected magnitude in the AB
system (W2*) (12)
201 I1 --- QS ? The manually assigned quality grade for
the photometry of SDSS images ranging from
0 for the poorest to 5 for the best
photometric quality (QS)
203 I1 --- QW ? The manually assigned quality grade for
the photometry of WISE images ranging from
0 for the poorest to 5 for the best
photometric quality (QW)
205- 212 F8.4 deg GLON Galactic longitude in galactic reference
frame (Glon)
214- 221 F8.4 deg GLAT Galactic latitude in galactic reference
frame (Glat)
223- 230 F8.4 deg SGL Supergalactic longitude in supergalactic
reference frame (SGL)
232- 239 F8.4 deg SGB Supergalactic latitude in supergalactic
reference frame (SGB)
241- 243 I3 --- Nkt Number of galaxies in the parent group
identified in KourKchi & Tully
2017ApJ...843...16K 2017ApJ...843...16K, Cat. J/ApJ/843/16
(Nkt)
245- 247 I3 --- N15 Number of galaxies in the parent group
identified in Tully 2015AJ....149..171T 2015AJ....149..171T,
Cat. J/AJ/149/171 (N15)
249- 256 F8.4 deg SGLg Supergalactic longitude of parent group in
the supergalactic frame of reference
(SGLg)
258- 265 F8.4 deg SGBg Supergalactic latitude of parent group in
the supergalactic frame of reference
(SGBg)
267- 271 I5 km/s Vgh The average velocity of the parent group in
heliocentric rest frame (Vgh)
273- 277 I5 km/s VgLS The average velocity of the parent group in
Local Sheet rest frame (VgLS)
279- 283 I5 km/s VgCMB The average velocity of the parent group in
CMB rest frame (VgCMB)
285- 289 F5.3 --- fg The cosmological correction factor fg
(fg) (13)
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Note (1): Taken from http://leda.univ-lyon1.fr/ and HYPERLEDA I. Catalog of
galaxies, Paturel et al. 2003A&A...412...45P 2003A&A...412...45P, Cat. VII/237.
Note (2): Quality flag as:
-16 = accepted, 9537 objects in our sample
0 = rejected as either > 3.5σ deviant or below the mass limit
of 109 M☉ or if the modulus uncertainty is larger
than 0.8 mag, 616 objects in our sample.
Note (3): The refering to the left-hand panel of Figure 16 of the
section 3 Zero-point calibration (DMriz).
Note (4): We use the optical data derived from the Gaussian propagation of
uncertainties in the associated measured quantities refering to
the section 4.1 Uncertainties.
Note (5): Refering to the right-hand panel of Figure 16 of the section 3
Zero-point calibration.
Note (6): We use the infrared data derived from the Gaussian propagation of
uncertainties in the associated measured quantities.
Note (7): Assuming the mass-to-light ratio Υ*W1 defined by the fit
shown in Figure 13 of the section 2.7 Extension to the infrared band.
Note (8): Where MHI is the atomic hydrogen mass as defined in the section
2.1 Gas mass, mass gas mainly included H I and He mass contributions.
Note (9): Mb is as defined in the equation 2 of the section 2 THE BTFR
formalism.
Note (10): The fj for galaxy j with distance dj accounts for the cosmic
curvature as defined in the section 2.3 H I flux bias following the
formula from Visser 2004CQGra..21.2603V 2004CQGra..21.2603V.
Note (11): Calculated from Wimx = Wmx/sin(i) where i is the inclination
angle, Wmx is derived from a measure of the 50 percentile width of
an observed H I profile adjusted for instrumental resolution and
redshift stretch effects, and statistically descriptive of the
peak-to-peak maximum rotation velocity of a galaxy as explained in
Courtois et al. 2009AJ....138.1938C 2009AJ....138.1938C, Cat. J/AJ/138/1938
and 2011MNRAS.414.2005C 2011MNRAS.414.2005C, Cat. J/MNRAS/414/2005.
Note (12): Corrected from Milky Way obscuration redshift k-correction and the
host dust attenuation with 0.05 mag uncertainty as refering in
section 2.2.2 of Kourkchi et al. 2020ApJ...902..145K 2020ApJ...902..145K,
Cat. J/ApJ/902/145.
Note (13): For galaxy group g calculated using the redshift of the parent group
which accounts for the cosmic curvature as defined in the
section 2.3 H I flux bias following the formula from
Visser 2004CQGra..21.2603V 2004CQGra..21.2603V.
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 06-Feb-2025