J/ApJ/902/145 Cosmicflows-4: Tully-Fisher distances (Kourkchi+, 2020)
Cosmicflows-4: the catalog of ∼10000 Tully-Fisher distances.
Kourkchi E., Tully R.B., Eftekharzadeh S., Llop J., Courtois H.M.,
Guinet D., Dupuy A., Neill J.D., Seibert M., Andrews M., Chuang J.,
Danesh A., Gonzalez R., Holthaus A., Mokelke A., Schoen D., Urasaki C.
<Astrophys. J., 902, 145 (2020)>
=2020ApJ...902..145K 2020ApJ...902..145K
ADC_Keywords: Galaxies; Photometry, ugriz; Radial velocities; H I data; Surveys
Keywords: Galaxy distances ; Spiral galaxies ; Galaxy photometry ;
Hubble constant ; H I line emission ;
Large-scale structure of the universe ; Inclination ; Sky surveys ;
Catalogs ; Distance measure ; Random Forests
Abstract:
We present the distances of 9792 spiral galaxies lying within
15000km/s using the relation between luminosity and rotation rate of
spiral galaxies. The sample is dominantly, but not exclusively, drawn
from galaxies detected in the course of the ALFALFA HI survey with the
Arecibo Telescope. Relations between HI line widths and luminosity are
calibrated at SDSS u, g, r, i, z bands and WISE W1 and W2 bands. By
exploiting secondary parameters, particularly color indices, we
address discrepancies between measured distances at different wave
bands with unprecedented detail. We provide a catalog that includes
reduced kinematic, photometric, and inclination parameters. We also
describe a machine-learning algorithm, based on the random forest
technique, that predicts the dust attenuation in spirals lacking
infrared photometry. We determine a Hubble Constant value of
H0=75.1±0.2(stat.), with potential systematics up to ±3km/s/Mpc.
Description:
We accept the HI line widths and fluxes from four resources: (1) Our
primary source (78% of cases) is the All Digital HI catalog (ADHI),
which has been collected over the course of the Cosmicflows program
(Courtois+ 2009, J/AJ/138/1938 ; 2011, J/MNRAS/414/2005 ;
A. Dupuy et al. 2020, in preparation) and is accessible online at the
Extragalactic Distance Database (EDD) website. (2) Most of the
remainder (19% of cases) are given by the Arecibo Legacy Fast ALFA
Survey (ALFALFA; Haynes+ 2011, J/AJ/142/170 ; 2018, J/ApJ/861/49) with
coverage over the decl. range 0<δ<+38°. (3) In a small
number of cases (50 galaxies, i.e., 0.5% of the total cases), line
widths are uniquely provided by the Springob/Cornell HI catalog
(Springob+ 2005, VIII/77). (4) For 3%, the source is the Pre Digital
HI catalog that is available in EDD, which provides information from
early analog HI line profiles, either from single beam or
interferometric observations (Fisher & Tully 1981ApJS...47..139F 1981ApJS...47..139F ;
Huchtmeier & Richter 1989, VIII/68).
We convert the HI flux within the 21cm line profiles, FHI, given in
the units Jy.km/s, to an HI magnitude, m21, using
m21=-2.5logFHI+17.40.
For the optical photometry of our galaxies, we use the SDSS DR12 data
release (see Cat. V/147). For each galaxy with available SDSS data, we
download all the single exposure cutouts at u, g, r, i, and z bands.
For the infrared part, we obtain the W1 (3.4um) and W2 (4.6um) images
of the WISE survey (see II/311), from the NASA/IPAC infrared science
archive (IRSA). All of our optical and infrared images are calibrated
to produce magnitudes in the AB system.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 499 10737 Data catalog: directly observed and adjusted data
and inferred parameters for spiral galaxies
used in this study
table4.dat 100 9792 Distance catalog
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See also:
VIII/68 : Huchtmeier-Richter HI catalog (Huchtmeier+ 1989)
VII/237 : HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)
VIII/77 : HI spectral properties of galaxies (Springob+, 2005)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)
V/154 : Sloan Digital Sky Surveys (SDSS), Release 16 (DR16) (Ahumada+, 2020)
J/AJ/112/2471 : The Ursa Major cluster. I. (Tully+ 1996)
J/ApJS/172/599 : SFI++ II. I-band Tully-Fisher catalog (Springob+, 2007)
J/AJ/138/1938 : EDD: All Digital HI profile catalog (Courtois+, 2009)
J/MNRAS/415/1935 : I-band photometry of cosmic flows (Courtois+, 2011)
J/MNRAS/414/2005 : Cosmic flows observations (Courtois+, 2011)
J/AJ/142/170 : ALFALFA survey: α.40 HI source catalog (Haynes+, 2011)
J/ApJ/765/94 : Calibration of the MIR Tully-Fisher relation (Sorce+, 2013)
J/AJ/146/86 : Cosmicflows-2 catalog (Tully+, 2013)
J/ApJ/792/129 : WISE W1/W2 Tully-Fisher relation calibrators (Neill+, 2014)
J/MNRAS/444/527 : Tully-Fisher distances for Spitzer galaxies (Sorce+, 2014)
J/MNRAS/445/2677 : Peculiar velocities in 6dFGS (Springob+, 2014)
J/AJ/152/50 : Cosmicflows-3 catalog (CF3) (Tully+, 2016)
J/ApJ/861/49 : ALFALFA extragalactic HI source catalog (Haynes+, 2018)
J/MNRAS/487/2061 : Distances for 2062 nearby spiral galaxies (Hong+, 2019)
J/ApJ/884/82 : SDSS, WISE & HI data of local spiral gal. (Kourkchi+, 2019)
J/ApJ/876/85 : HST observations for LMC Cepheids (Riess+, 2019)
J/ApJ/896/3 : Cosmicflows-4: Tully-Fisher relations (Kourkchi+, 2020)
http://edd.ifa.hawaii.edu/ : The Extragalactic Distance Database home page
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 I7 --- PGC [2/6724508] Principal Galaxies Catalog ID in
HyperLEDA (G1)
9- 33 A25 --- Name Common name
35- 36 I2 deg Inc [45/90] Measured inclination of the galaxy
38- 39 I2 deg e_Inc [1/23] Uncertainty in Inc
41- 45 I5 km/s HRV [-274/19518] Heliocentric velocity from HI
observations
47- 49 I3 km/s Wmx [15/909] Adjusted HI line width (2)
51- 53 I3 km/s e_Wmx [5/186] Uncertainty in Wmx
55- 59 F5.3 [km/s] logWmxi [1.2/3] Log of inclination corrected Wmx (2)
61- 65 F5.3 [km/s] e_logWmxi [0.003/0.8] Uncertainty in logWmxi
67- 72 F6.3 mag m21 [9.14/38.4] HI 21cm magnitude (3)
74- 78 F5.3 mag e_m21 [0/0.26] Uncertainty in m21
80- 84 F5.2 mag umag [0/20.8]? Apparent u band AB magnitude (4)
86- 90 F5.2 mag gmag [0.78/19.12]? Apparent g band AB magnitude (4)
92- 96 F5.2 mag rmag [0.67/18.72]? Apparent r band AB magnitude (4)
98- 102 F5.2 mag imag [0.9/19.94]? Apparent i band AB magnitude (4)
104- 108 F5.2 mag zmag [0/18.91]? Apparent z band AB magnitude (4)
110- 116 F7.2 mag W1mag [-100/18.4]? WISE 3.26 micron band apparent
AB magnitude (4)
118- 124 F7.2 mag W2mag [-100/41]? WISE 4.62 micron band apparent AB
magnitude (4)
126- 129 F4.2 --- (b/a)s [0.07/1]? Axial ratio from SDSS image (5)
131- 134 F4.2 --- (b/a)W [0.07/1]? Axial ratio from WISE image (5)
136- 140 F5.2 arcmin Reu [-0.02/4.7]? Half light semi-major axis in u
band
142- 145 F4.2 arcmin Reg [0.05/3.9]? Half light semi-major axis in g
band
147- 151 F5.2 arcmin Rer [-0.02/3.6]? Half light semi-major axis in r
band
153- 156 F4.2 arcmin Rei [0.05/3.4]? Half light semi-major axis in i
band
158- 162 F5.2 arcmin Rez [-0.02/3.2]? Half light semi-major axis in z
band
164- 168 F5.2 arcmin ReW1 [-0.02/12.4]? Half light semi-major axis in
WISE 3.26 micron band
170- 174 F5.2 arcmin ReW2 [-0.02/9.63]? Half light semi-major axis in
WISE 4.62 micron band
176- 180 F5.2 mag ucmag [0/20.6]? Corrected u band AB magnitude (6)
182- 186 F5.2 mag gcmag [0.6/18.9]? Corrected g band AB magnitude (6)
188- 192 F5.2 mag rcmag [0.57/18.7]? Corrected r band AB magnitude (6)
194- 198 F5.2 mag icmag [0.86/18.9]? Corrected i band AB magnitude (6)
200- 204 F5.2 mag zcmag [0/18.8]? Corrected z band AB magnitude (6)
206- 210 F5.2 mag W1cmag [0.05/18.4]? Corrected WISE 3.26 micron band
AB magnitude (6)
212- 216 F5.2 mag W2cmag [0.02/41.1]? Corrected WISE 4.62 micron band
AB magnitude (6)
218- 221 F4.2 mag Au [0/1.82]? u band dust attenuation correction
223- 226 F4.2 mag e_Au [0/2.4]? Uncertainty in Au
228- 231 F4.2 mag Ag [0/1.41]? g band dust attenuation correction
233- 236 F4.2 mag e_Ag [0/2.4]? Uncertainty in Ag
238- 241 F4.2 mag Ar [0/1.16]? r band dust attenuation correction
243- 246 F4.2 mag e_Ar [0/2.3]? Uncertainty in Ar
248- 251 F4.2 mag Ai [0/0.98]? i band dust attenuation correction
253- 256 F4.2 mag e_Ai [0/2.3]? Uncertainty in Ai
258- 261 F4.2 mag Az [0/0.82]? z band dust attenuation correction
263- 266 F4.2 mag e_Az [0/2.17]? Uncertainty in Az
268- 272 F5.2 mag AW1 [-1.01/0.96]? WISE 3.26 micron band dust
attenuation correction
274- 277 F4.2 mag e_AW1 [0/2]? Uncertainty in AW1
279- 283 F5.2 mag AW2 [-1.31/1.04]? WISE 4.62 micron band dust
attenuation correction
285- 288 F4.2 mag e_AW2 [0/2]? Uncertainty in AW2
290- 294 F5.2 mag u*mag [-1.62/20.1]? Dust corrected u band AB
magnitude (7)
296- 300 F5.2 mag g*mag [0.6/18.7]? Dust corrected g band AB
magnitude (7)
302- 306 F5.2 mag r*mag [0.57/18.5]? Dust corrected r band AB
magnitude (7)
308- 312 F5.2 mag i*mag [0.86/18.71]? Dust corrected i band AB
magnitude (7)
314- 318 F5.2 mag z*mag [-0.6/18.74]? Dust corrected z band AB
magnitude (7)
320- 324 F5.2 mag W1*mag [0.05/18.6]? Dust corrected WISE 3.26 micron
band AB magnitude (7)
326- 330 F5.2 mag W2*mag [0.02/41.1]? Dust corrected WISE 4.62 micron
band AB magnitude (7)
332- 336 F5.2 mag pW2*mag [0/41.1] Predicted value for the corrected
W2-band magnitude (8)
338- 343 F6.2 mag Gu [0/156.3]? u band host dust attenuation factor
345- 350 F6.2 mag Gg [0/155.7]? g band host dust attenuation factor
352- 357 F6.2 mag Gr [0/142.4]? r band host dust attenuation factor
359- 364 F6.2 mag Gi [0/142.1]? i band host dust attenuation factor
366- 371 F6.2 mag Gz [0/128]? z band host dust attenuation factor
373- 377 F5.2 mag Gw1 [0/24.8]? WISE 3.26 micron band host dust
attenuation factor
379- 382 F4.2 mag Gw2 [0/8]? WISE 4.62 micron band host dust
attenuation factor
384- 389 F6.2 mag pGu [0/156.3]? Predicted u band host dust
attenuation factor
391- 396 F6.2 mag pGg [0/156]? Predicted g band host dust
attenuation factor
398- 403 F6.2 mag pGr [0/142.4]? Predicted r band host dust
attenuation factor
405- 410 F6.2 mag pGi [0/142.1]? Predicted i band host dust
attenuation factor
412- 417 F6.2 mag pGz [0/128]? Predicted z band host dust
attenuation factor
419- 423 F5.2 mag pGW1 [0/24.8]? Predicted W1 dust attenuation factor
425- 428 F4.2 mag pGW2 [0/8]? Predicted W2 dust attenuation factor
430- 434 F5.2 mag pA-u [0/51.2]? Predicted u band dust extinction
of host
436- 440 F5.2 mag pA-g [0/51.1]? Predicted g band dust extinction
of host
442- 446 F5.2 mag pA-r [0/46.7]? Predicted r band dust extinction
of host
448- 452 F5.2 mag pA-i [0/46.6]? Predicted i band dust extinction
of host
454- 458 F5.2 mag pA-z [0/42]? Predicted z band dust extinction of
host
460- 463 F4.2 mag pA-W1 [0/8]? Predicted WISE 3.26 micron band dust
extinction of host
465- 468 F4.2 mag pA-W2 [0/2.6]? Predicted WISE 4.62 micron band
dust extinction of host
470- 475 F6.2 --- P1-W2 [-24.5/14.82]? Principal component,
calculated at W2 band, Equation 4
477- 480 F4.2 --- e_P1-W2 [0.04/2.3]? Uncertainty in P1-W2
482- 487 F6.2 --- P1-pW2 [-24.5/14.82]? Principal component,
predicted at W2 band
489- 493 F5.2 --- P1-W1 [-5.9/13.8]? Principal component, calculated
at W1 band (9)
495 I1 --- QSflag [0/5] Quality flag, SDSS images
(5=best quality) (10)
497 I1 --- QWflag [0/5] Quality flag, WISE images
(5=best quality) (10)
499 I1 --- Rsrc [0/2] Source of the adopted attenuation
parameter (11)
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Note (2): Observed linewidths at 50% average HI flux are corrected for
spectral resolution and redshift and further adjusted to approximate
twice (projected) maximum rotation, Wmx. The parameter de-projected to
edge-on orientation is Wmxi=Wmx/sin(Inc).
Note (3): Calculated from the HI flux, FHI, using m21=-2.5log(FHI)+17.4.
Note (4): Total raw magnitudes. The uncertainty on the measured u-band
magnitudes are ∼0.1mag. The uncertainties on all other measured
magnitudes are not worse than 0.05 mag, which is conservatively adopted
for the purpose of error propagation in this study.
Note (5): Where a and b are the semi-major and semi-minor axes of the
elliptical aperture, respectively.
Note (6): Corrected for Milky Way obscuration, redshift k-correction, and
aperture effects, but not the inclination dependent dust attenuation,
based on the corresponding raw magnitude,
mc=mtotal-Ab-Ak-Aa.
Note (7): Correcting for the effect of global dust obscuration,
m*=mtotal-Ab-Ak-Aa-Ai.
Note (8): The predicted value for the W2-band magnitude based on the optical
photometry and other observable features of the galaxy (discussed in the
Appendix B).
Note (9): The main principal component derived for W1-band. This parameter
is useful for galaxies with poor W2-band photometry. P1,W2 is
approximated by 1.021P1,W1-0.094, Kourkchi+ (2019, J/ApJ/884/82).
Note (10): The manually assigned quality for the photometry of SDSS and
WISE images. The quality grade ranges from 0 for the poorest quality (or
missing data) to 5 for the best quality.
Note (11): An integer number between 0 and 2 that specifies what parameters
are used for calculation of the dust obscuration in the host galaxies --
0 = uses the predicted W2*mag;
1 = uses the observed W1-band magnitude;
2 = uses the W2-band through the standard attenuation formulation as
discussed in Section 2.2.2.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 I7 --- PGC [2/6724508] Principal Galaxies Catalog ID in
HyperLEDA (G1)
9- 13 I5 km/s Vls [-355/19807] Radial velocity in the frame of
the Local Sheet
15- 19 I5 km/s Vcmb [-462/19177] Radial velocity in the CMB frame
21- 25 F5.3 --- f [0.99/1.05] Cosmological correction term (1)
27- 31 F5.2 mag DMbest [24.37/38.6]? Best distance modulus
33- 36 F4.2 mag e_DMbest [0.1/6.51]? Uncertainty in DMbest
38- 42 F5.2 mag DM-r [27.6/38.6]? Adjusted/Regularized r band
distance modulus
44- 47 F4.2 mag e_DM-r [0.12/6.3]? Uncertainty in DM-r
49- 52 F4.2 --- RMS-r [0.3/0.6]? RMS scatter of moduli deviations
about the r-band TFR
54- 58 F5.2 mag DM-i [27.69/38.61]? Adjusted/Regularized i band
distance modulus
60- 63 F4.2 mag e_DM-i [0.12/6.51]? Uncertainty in DM-i
65- 68 F4.2 --- RMS-i [0.39/0.6]? RMS scatter of moduli deviations
about the i-band TFR
70- 74 F5.2 mag DM-z [28/38.64]? Adjusted/Regularized z band
distance modulus
76- 79 F4.2 mag e_DM-z [0.12/6.7]? Uncertainty in DM-z
81- 84 F4.2 --- RMS-z [0.4/0.6]? RMS scatter of moduli deviations
about the z-band TFR
86- 90 F5.2 mag DM-W1 [18/37.5]? Adjusted/Regularized W1 band
distance modulus
92- 95 F4.2 mag e_DM-W1 [0.1/3.3]? Uncertainty in DM-W1
97- 100 F4.2 --- RMS-W1 [0.48/0.7]? RMS scatter of moduli deviations
about the W1-band TFR
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Note (1): The cosmological correction term is:
f=1+1/2[1-q0]z-1/6[1-q0-3q02+j0]z2
where j0=1, and q0=1/2(Ωm-2ΩΛ)=-0.595
assuming Ωm=0.27, Ωm+ΩΛ=1, and
z=VLS/c (Wright 2006PASP..118.1711W 2006PASP..118.1711W).
See footnote 15.
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Global notes:
Note (G1): HyperLEDA, http://leda.univ-lyon1.fr/,
Paturel et al. (2003, VII/237), Makarov et al. (2014A&A...570A..13M 2014A&A...570A..13M)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 21-Apr-2022