J/ApJS/261/21 HI emission line profile of ALFALFA nearby galaxies (Yu+, 2022)
Statistical analysis of HI profile asymmetry and shape for nearby galaxies.
Yu N., Ho L.C., Wang J., Li H.
<Astrophys. J. Suppl. Ser., 261, 21 (2022)>
=2022ApJS..261...21Y 2022ApJS..261...21Y
ADC_Keywords: Galaxies, nearby; H I data; Redshifts; Optical; Surveys
Keywords: Disk galaxies ; Interstellar medium ; Interstellar atomic gas
Abstract:
We present a uniform analysis of the integrated profile of the HI
emission line of 29958 nearby (z<0.06) galaxies extracted from the
ALFALFA 21cm survey. We apply the curve-of-growth technique to derive
a database of spectral parameters and robust estimates of their
associated uncertainties. Besides the central velocity and total flux,
the main catalog provides new measures of line width, profile
asymmetry, and profile shape. For a subsample of 13511 galaxies with
optical properties available from the Sloan Digital Sky Survey, we
compute inclination angle-corrected line widths, rotation velocities
empirically calibrated from spatially resolved observations, and
dynamical masses based on HI sizes estimated from the HI mass. To
facilitate subsequent scientific applications of the database, we also
compile a number of ancillary physical properties of the galaxies,
including their optical morphology, stellar mass, and various
diagnostics of star formation activity. We use the homogeneous catalog
of HI parameters to examine the statistical properties of profile
asymmetry and shape. Across the full sample, which covers a wide range
of stellar masses and environments, statistically significant HI
profile asymmetry is detected in ∼20% of the galaxy population. The
global HI profiles are 35.2%±0.3% single-peaked, 26.9%±0.3%
flat-topped, and 37.9%±0.3% double-horned. At a given inclination
angle, double-horned profiles are preferentially associated with
galaxies of higher stellar mass or optical concentration, while
galaxies of lower mass or concentration tend to have single-peaked
profiles.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 158 29958 Parameters derived from the HI spectra of the
main sample
table3.dat 123 13511 Properties of the SDSS subsample
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See also:
VII/26 : Uppsala General Catalogue of Galaxies (UGC) (Nilson 1973)
VIII/73 : HI Parkes All Sky Survey Catalogue (HIPASS) (Meyer+, 2004)
VIII/77 : HI spectral properties of galaxies (Springob+, 2005)
VIII/89 : Northern HI Parkes All Sky Survey Catalogue (HIPASS) (Wong+, 2006)
V/154 : Sloan Digital Sky Surveys (SDSS), Release 16 (DR16) (Ahumada+, 2020)
J/AJ/114/2402 : Rotation curves of early-type galaxies (Courteau+, 1997)
J/A+A/370/765 : HI synthesis observations in UMa cluster (Verheijen+, 2001)
J/AJ/128/16 : HIPASS Bright Galaxy Catalog (Koribalski+, 2004)
J/A+A/438/507 : Degree of lopsidedness for galaxies (Bournaud+, 2005)
J/A+A/435/459 : HI data of edge-on spiral galaxies (Huchtmeier+, 2005)
J/ApJ/653/240 : Low-mass SDSS dwarf galaxy properties (Geha+, 2006)
J/AJ/133/2569 : Arecibo legacy fast ALFA survey III. (Giovanelli+, 2007)
J/ApJ/655/144 : ACS Virgo Cluster Survey. XIII. (Mei+, 2007)
J/ApJS/172/599 : SFI++ II. A new I-band Tully-Fisher cat. (Springob+, 2007)
J/MNRAS/403/683 : GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)
J/MNRAS/415/431 : Galaxies with wide HI profiles (Brosch+, 2011)
J/A+A/532/A117 : AMIGA VIII. Flux ratio asymmetry parameter (Espada+, 2011)
J/AJ/142/170 : ALFALFA survey: α.40 HI source catalog (Haynes+, 2011)
J/A+A/544/A65 : GALEX Arecibo SDSS survey. VI. (Catinella+, 2012)
J/MNRAS/436/34 : GALEX Arecibo SDSS survey. Final release (Catinella+, 2013)
J/AJ/146/86 : Cosmicflows-2 catalog (Tully+, 2013)
J/AJ/152/157 : Mass models for 175 disk galaxies with SPARC (Lelli+, 2016)
J/MNRAS/460/2143 : HI size-mass relation of galaxies (Wang+, 2016)
J/MNRAS/476/875 : xGASS catalog (Catinella+, 2018)
J/ApJ/861/49 : ALFALFA extragalactic HI source catalog (Haynes+, 2018)
J/A+A/632/A78 : A case study of the HI content of HCG 16 (Jones+, 2019)
J/AJ/160/271 : ∼30000 galaxies with ALFALFA-SDSS (Durbala+, 2020)
J/ApJ/898/102 : Rot. vel. & dynamical mass of gal. from HI sp. (Yu+, 2020)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [AGC]
5- 10 I06 --- AGC Galaxy name from the Arecibo General Cat. (G1)
12- 20 F9.5 deg RAdeg Right Ascension, optical counterpart (J2000)
22- 29 F8.5 deg DEdeg Declination, optical counterpart (J2000)
31- 35 F5.1 Mpc Dist [0.3/257.5] Luminosity distance from
the ALFALFA catalog
37- 40 F4.1 Mpc e_Dist [0/31] Uncertainty in Dist
42- 46 I5 km/s Vc [-418/17669] Flux intensity-weighted
central velocity
48- 49 I2 km/s e_Vc [3/89] Uncertainty in Vc
51- 57 F7.2 Jy.km/s HIflux [0.14/8831] Total integrated flux of
the HI line
59- 65 F7.2 Jy.km/s e_HIflux [0.03/1397] Uncertainty in HIflux
67- 74 A8 km/s W85 Velocity width measured at 85% of the total
line flux
76- 78 I3 km/s e_W85 [1/127] Uncertainty in W85
80- 83 F4.2 --- Af [1/8.82] Integrated flux asymmetry (1)
85- 88 F4.2 --- e_Af [0/2.72] Uncertainty in Af
90- 94 F5.2 --- Ac [1/75.72] Flux distribution asymmetry (1)
96-100 F5.2 --- e_Ac [0/16.71] Uncertainty in Ac
102-106 F5.2 --- Cv [1.25/13.73] Profile concentration
108-111 F4.2 --- e_Cv [0.13/0.7] Uncertainty in Cv
113-118 F6.3 --- K [-0.42/0.31] Profile shape
120-124 F5.3 --- e_K [0.015/0.15] Uncertainty in Kappa
126-132 F7.1 --- S/N [1.7/22731] Signal-to-noise of profile
134-137 F4.1 --- sigma [0.4/14] Noise level of the profile
139-143 F5.2 [Msun] logMHI [4/11] HI mass (2)
145-148 F4.2 [Msun] e_logMHI [0.07/0.5] Uncertainty in logMHI
150-158 A9 --- Notes Notes for the HI spectra (3)
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Note (1): The asymmetry parameter AF is defined as the larger of the ratios
of the integrated flux of one side of the line relative to the other,
while AC is the larger of the ratios of the slopes of the rising part
of the curve-of-growth (CoG; Yu+ 2020, J/ApJ/898/102) of the two sides.
Note (2): Following MHI=2.36*105 Dist2 * FHI in solar units,
Roberts (1962AJ.....67..437R 1962AJ.....67..437R); for a distance uncertainty of 10% and a
flux uncertainty of 15%, the typical uncertainty of logMHI is 0.11dex.
Note (3): Notes as follows:
1 = code 1 detection;
2 = code 2 detection;
r = there are data points with spectral weight less than 0.5, which are
located at the edge of the emission signal;
c = the HI emission overlaps with that of nearby companion(s);
p = the HI emission is not confused even though there is at least a
projected neighbor within the Arecibo beam.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [AGC]
5- 10 I6 --- AGC Galaxy name from Arecibo General Cat. (G1)
12- 18 F7.5 --- z [0.01/0.06] Optical redshift from SDSS
20- 23 F4.1 kpc R90 [0.7/66] Radius containing 90% of the
Petrosian flux in the r band
25- 28 F4.1 kpc e_R90 [0/44.2] Uncertainty in R90
30- 33 F4.1 kpc RHI [2.3/88] HI Radius (1)
35- 38 F4.1 kpc e_RHI [0.4/13.2] Uncertainty in RHI
40- 42 F3.1 --- C [1/6] Optical (r-band) concentration index
44- 46 F3.1 --- b/a [0.1/1] Axis ratio in the r band
48- 49 I2 deg i [10/90] Optical inclination angle
51- 52 I2 deg e_i [5/20] Uncertainty in i
54- 57 I4 km/s Vrot [18/1242] Rotation velocity (2)
59- 62 I4 km/s e_Vrot [1/1242] Uncertainty in Vrot
64- 70 F7.3 [Msun] logMstar [7.5/11.7]?=-99 Stellar mass (3)
72- 78 F7.3 [Msun] e_logMstar [0.001/0.3]?=-99 Uncertainty in logMstar
80- 86 F7.3 [Msun/yr] logSFR [-3.15/1.5]?=-99 Star formation rate (3)
88- 94 F7.3 [Msun/yr] e_logSFR [0.001/1.4]?=-99 Uncertainty in logSFR
96- 102 F7.3 [Msun/yr] logSFRin [-3.53/4]?=-99 Star formation rate within
the 3"-diameter SDSS fiber (4)
104- 107 F4.2 --- Dn4000 [0/3.1] 4000 Angstrom break strength (4)(5)
109- 114 F6.2 0.1nm EWHa [-4.6/527] Equivalent width of Halpha
emission line (4)
116- 119 F4.1 [Msun] logMdyn [8.7/13.2] Dynamical mass within RHI
121- 123 F3.1 [Msun] e_logMdyn [0.1/0.9] Uncertainty in logMdyn
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Note (1): Calculated from the HI mass-size relation of
Wang+ (2016, J/MNRAS/460/2143)
Note (2): While calculating the rotation velocity, we assume the minimum
inclination angle is 10 degree.
Note (3): Stellar mass and SFR from spectral energy distribution fitting
(Salim+ 2018ApJ...859...11S 2018ApJ...859...11S), scaled to the distance of ALFALFA.
Note (4): SFRin, Dn4000, and EWHa are from the MPA-JHU catalog, calculated
within the central 3 arcsecond fiber of SDSS. SFRin is scaled to the
distance of ALFALFA and converted to the initial mass function of
Chabrier (2003PASP..115..763C 2003PASP..115..763C).
Note (5): Dn4000 is the ratio of the average flux density at 4000-4100Å to
that at 3850-3950Å, Balogh+ (1999ApJ...527...54B 1999ApJ...527...54B).
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Global note:
Note (G1): UGC/AGC numbers from a private database of extragalactic objects
maintained by M.P. Haynes and R. Giovanelli (see Cat. VIII/77). The
AGC entry normally corresponds to the optical counterpart of the HI source.
Numbers lower than 100,000 are UGC numbers (Cat. VII/26).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 23-Sep-2022