J/ApJ/777/42 Kinematic and HI data for the NFGS (Kannappan+, 2013)
Connecting transitions in galaxy properties to refueling.
Kannappan S.J., Stark D.V., Eckert K.D., Moffett A.J., Wei L.H.,
Pisano D.J., Baker A.J., Vogel S.N., Fabricant D.G., Laine S., Norris M.A.,
Jogee S., Lepore N., Hough L.E., Weinberg-Wolf J.
<Astrophys. J., 777, 42 (2013)>
=2013ApJ...777...42K 2013ApJ...777...42K
ADC_Keywords: Galaxies, nearby ; H I data ; Photometry, SDSS ;
Photometry, ultraviolet ; Photometry, infrared
Keywords: galaxies: evolution
Abstract:
We relate transitions in galaxy structure and gas content to
refueling, here defined to include both the external gas accretion and
the internal gas processing needed to renew reservoirs for star
formation. We analyze two z=0 data sets: a high-quality ∼200 galaxy
sample (the Nearby Field Galaxy Survey, data release herein) and a
volume-limited ∼3000 galaxy sample with reprocessed archival data.
Both reach down to baryonic masses ∼109M☉ and span
void-to-cluster environments. Two mass-dependent transitions are
evident: (1) below the "gas-richness threshold" scale (V∼125km/s),
gas-dominated quasi-bulgeless Sd-Im galaxies become numerically
dominant; while (2) above the "bimodality" scale (V∼200km/s),
gas-starved E/S0s become the norm. Notwithstanding these transitions,
galaxy mass (or V as its proxy) is a poor predictor of gas-to-stellar
mass ratio Mgas/M*. Instead, Mgas/M* correlates well with the
ratio of a galaxy's stellar mass formed in the last Gyr to its
preexisting stellar mass, such that the two ratios have numerically
similar values. This striking correspondence between past-averaged
star formation and current gas richness implies routine refueling of
star-forming galaxies on Gyr timescales. We argue that this refueling
underlies the tight Mgas/M* versus color correlations often used
to measure "photometric gas fractions." Furthermore, the threshold and
bimodality scale transitions reflect mass-dependent demographic shifts
between three refueling regimes--accretion-dominated,
processing-dominated, and quenched. In this picture, gas-dominated
dwarfs are explained not by inefficient star formation but by
overwhelming gas accretion, which fuels stellar mass doubling in
≲1Gyr. Moreover, moderately gas-rich bulged disks such as the Milky
Way are transitional, becoming abundant only in the narrow range
between the threshold and bimodality scales.
Description:
Our analysis relies on two samples. The highest-quality HI data,
multi-band photometry, and kinematic data come from the Nearby Field
Galaxy Survey (NFGS; Jansen et al. 2000, J/ApJS/126/331; 2000,
J/ApJS/126/271; Kannappan & Fabricant 2001AJ....121..140K 2001AJ....121..140K; Kannappan
et al. 2002AJ....123.2358K 2002AJ....123.2358K; Wei et al. 2010, J/ApJ/708/841), a broadly
representative sample of ∼200 galaxies spanning stellar masses
M*∼108-1012M☉ and all morphologies. Better statistics are
offered by a volume-limited sample of ∼3000 galaxies, with
flux-limited HI data and partial kinematic information from the blind
21cm Arecibo Legacy Fast ALFA (ALFALFA; Giovanelli et al.
2005AJ....130.2598G 2005AJ....130.2598G; Haynes et al. 2011, J/AJ/142/170) survey.
The HI data set presented in Table 2 expands on that of Wei et al.
(W10a; 2010, J/ApJ/708/841) with 30 new Robert C. Byrd Green Bank
Telescope (GBT) 21cm observations taken for the Nearby Field Galaxy
Survey (NFGS) under program GBT10A-070 in 2010 January, February, and
July (PI: Kannappan). We add these to the 27 GBT observations obtained
by W10a under programs GBT07A-072 and GBT07C-148 in 2007 March and
October.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 166 190 Photometry and stellar mass estimates
table2.dat 121 190 Kinematic and HI data for the Nearby Field
Galaxy Survey (NFGS)
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See also:
II/312 : GALEX-DR5 (GR5) sources from AIS and MIS (Bianchi+ 2011)
VII/259 : 6dF galaxy survey final redshift release (Jones+, 2009)
II/294 : The SDSS Photometric Catalog, Release 7 (Adelman-McCarthy+, 2009)
VII/246 : GOODS Morphological Catalog (Bundy+, 2005)
VII/237 : HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)
J/ApJ/769/82 : H2 masses in a broad sample of galaxies (Stark+, 2013)
J/ApJ/744/44 : Hα and UV fluxes in nearby galaxies (Weisz+, 2012)
J/AJ/142/170 : ALFALFA survey: the α.40 HI source catalog (Haynes+, 2011)
J/MNRAS/414/3699 : Study of hot stellar systems and galaxies (Misgeld+, 2011)
J/ApJ/733/L47 : Galaxy bulge types within 11Mpc (Fisher+, 2011)
J/MNRAS/413/971 : Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)
J/ApJS/192/6 : A GALEX UV imaging survey of nearby galaxies (Lee+, 2011)
J/PASP/122/1397 : Spitzer Survey of Stellar Structure in Gal. (Sheth+, 2010)
J/MNRAS/405/1089 : Photometric scaling for L/S0 galaxies (Laurikainen+ 2010)
J/MNRAS/403/683 : GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)
J/ApJ/711/284 : Galaxy Zoo: AGN host galaxies (Schawinski+, 2010)
J/ApJ/708/841 : Star formation in E/S0 galaxies (W10a) (Wei+, 2010)
J/MNRAS/396/818 : Blue early-type galaxies in Galaxy Zoo (Schawinski+, 2009)
J/PASP/117/227 : Properties of 101 galaxies from the NFGS (Kewley+, 2005)
J/AJ/127/3273 : Nearby galaxies HI observations (Vogt+, 2004)
J/AJ/127/2002 : Star Formation Rate of NFGS galaxies (Kewley+, 2004)
J/A+A/405/5 : Catalogue of ISM content of normal galaxies (Bettoni+, 2003)
J/A+A/373/24 : Blue compact galaxies from SBS (Pustilnik+ 2001)
J/ApJS/126/331 : Spectrophotometry from NFGS (Jansen+ 2000)
J/ApJS/126/271 : Surface photometry from NFGS (Jansen+ 2000)
J/PASP/111/438 : Updated Zwicky catalog (UZC) (Falco+, 1999)
J/AJ/114/1365 : Physical properties of stellar systems (Burstein+, 1997)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- NFGS [1/198] The NFGS ID number
5- 13 A9 --- Name Object name
15- 20 F6.3 mag NUV [14/19.1]? GALEX NUV magnitude (1)
22- 26 F5.3 mag e_NUV ? Error in NUV
28- 33 F6.3 mag umag [12.6/16.3]? SDSS u band magnitude (1)
35- 39 F5.3 mag e_umag ? Error in umag
41- 46 F6.3 mag gmag [11.2/15.1]? SDSS g band magnitude (1)
48- 52 F5.3 mag e_gmag ? Error in gmag
54- 59 F6.3 mag rmag [10.4/14.5]? SDSS r band magnitude (1)
61- 65 F5.3 mag e_rmag ? Error in rmag
67- 72 F6.3 mag imag [10.0/14.4]? SDSS i band magnitude (1)
74- 78 F5.3 mag e_imag ? Error in imag
80- 85 F6.3 mag zmag [9.9/14.3]? SDSS z band magnitude (1)
87- 91 F5.3 mag e_zmag ? Error in zmag
93- 98 F6.3 mag Jmag [8.8/13.5]? 2MASS J band magnitude (1)
100-104 F5.3 mag e_Jmag ? Error in Jmag
106-111 F6.3 mag Hmag [8.2/12.8]? 2MASS H band magnitude (1)
113-117 F5.3 mag e_Hmag ? Error in Hmag
119-124 F6.3 mag Ksmag [7.8/13.1]? 2MASS Ks band magnitude (1)
126-130 F5.3 mag e_Ksmag ? Error in Ksmag
132-137 F6.3 mag [3.6] [7.7/12.4]? Spitzer/IRAC 3.6um band magnitude
139-143 F5.3 mag e_[3.6] ? Error in [3.6]
145-149 F5.2 [Msun] M* [7.8/11.8] Log of stellar mass
151-155 F5.2 [Msun] MKGB Log of stellar mass from KGB (2)
157-160 F4.1 arcsec r50 [4.2/60]? SDSS-r 50% light radius rr50
162-166 F5.1 arcsec r90 [13/190]? SDSS r band 90% light radius
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Note (1): With foreground extinction corrections determined from the
Schlegel et al. (1998ApJ...500..525S 1998ApJ...500..525S) dust maps using the extinction
curves of O'Donnell (1994ApJ...422..158O 1994ApJ...422..158O) and Cardelli et al.
(1989ApJ...345..245C 1989ApJ...345..245C) in the optical and UV, respectively. We also
assume an effective wavelength of 2271Å for the GALEX NUV filter.
Note (2): Masses from KGB: Kannappan et al. (2009AJ....138..579K 2009AJ....138..579K); masses
not used in this paper.
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- NFGS [1/198] The NFGS ID number
5- 9 F5.1 deg PA1 ]0/180]? Slit position angle of observation used
to derive ionized gas rotation curve
10 A1 --- u_PA1 [*] Estimated PA1 (3)
12- 16 F5.1 deg PA2 ]0/180]? Slit position angle of observation used
to derive stellar absorption line kinematics
17 A1 --- u_PA2 [*] Estimated PA2 (3)
19- 22 F4.1 deg i [0/90] Inclination
24- 27 F4.1 deg i2 [0/90]? Inclination estimates from KFF (4)
29- 31 I3 km/s Vpmm [3/333]? Maximum rotation velocity Vpmm (5)
32 A1 --- u_Vpmm Uncertainty flag on Vpmm
34- 37 F4.1 arcsec Re [4/64.6] Half-light radius in the B band (6)
39- 42 F4.1 arcsec Ext [4.5/93]? Extent of the gas rotation curve
44- 47 F4.1 % Asym [0.6/47.4]? Asymmetry of the gas rotation curve
49- 51 I3 km/s W50 [46/708]? The equivalent W50 linewidth
53- 55 I3 km/s e_W50 [2/143]? W50 uncertainty
57- 58 A2 --- u_W50 []d ] "]": unreliable linewidth (3)
60- 63 A4 --- r_W50 [W10a] W10a: Wei et al., 2010, J/ApJ/708/841 (7)
65- 67 I3 km/s sigma [22/341]? Stellar dispersion (σre/4)
69- 70 I2 km/s e_sigma [7/30]? sigma uncertainty
72 A1 --- u_sigma [l] possible unreliable sigma (3)
74- 76 I3 km/s V* [14/306]? Stellar rotation velocity (8)
78- 80 I3 km/s V [31/483]? Characteristic internal velocity (9)
82- 84 I3 km/s e_V ? V uncertainty
85 A1 --- u_V []] "]" = unreliable linewidth (Section 2.1.3)
87- 88 A2 --- r_V Origin of V (10)
90 A1 --- l_logMHI Limit flag on logMHI
92- 96 F5.2 [Msun] logMHI [6.02/10.7]? Log of HI mass (11)
98-101 F4.2 [Msun] e_logMHI ? logMHI uncertainty
102-104 A3 --- u_logMHI [ ,Ddk] Possible confusion (3)
106-109 A4 --- r_logMHI [W10a] W10a: Wei et al., 2010, J/ApJ/708/841 (7)
111-115 I5 km/s Vmin [522/12500]? Lower range of heliocentric
velocity (12)
117-121 I5 km/s Vmax [0/13076]? Upper range of heliocentric
velocity (12)
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Note (3): Flag as follows:
k = HI data from ALFALFA survey, with upper limits estimated from the survey
sensitivity limit (Haynes et al. 2011, J/AJ/142/170).
l = Stellar velocity dispersion may be an unreliable metric of
characteristic velocity V, based on either late-type morphology
or low dispersion (Section 2.1.3).
* = P.A. uncertain or slit P.A. misaligned by more than 10° with the
galaxy major axis.
d = Confirmed likely confused; HI flux corrected as described in
Section 2.1.2 and HI linewidth designated as unreliable.
D = Literature HI data possibly subject to confusion based on identification
of a close companion or ongoing interaction/merger by KFF.
dd = Linewidth inconsistent with much larger ALFALFA value; both come from
low-S/N (∼6) spectra and are inconsistent with the Tully-Fisher relation.
Note (4): Inclination estimates from KFF (Kannappan+, 2002AJ....123.2358K 2002AJ....123.2358K),
usually inferior except for UGC 9562 and NGC 3499, for which the new
estimate applies only to the gas, not the stars.
Note (5): For ionized gas rotation velocities, we adopt a non-parametric
statistical estimator of the maximum rotation velocity, the "probable
min-max" Vpmm of Raychaudhury et al. (1997AJ....113.2046R 1997AJ....113.2046R) as
implemented in KFF (Kannappan+, 2002AJ....123.2358K 2002AJ....123.2358K). Uncertainties
on Vpmm are set to 11km/s following KFF (See Section 2.1.3).
Note (6): Half-light radius in the B band from Jansen et al. 2000
(J/ApJS/126/271), converted from the authors' geometric mean aperture
radius convention to a major axis radius convention. This B-band
radius is denoted re as distinct from the r-band half-light radius
denoted rr50 in Table 1.
Note (7): We have further augmented the 21cm inventory for the Nearby Field
Galaxy Survey (NFGS) using the literature compilation of W10a (Wei et
al., 2010, J/ApJ/708/841); not duplicated in this table. See section
2.1.2.
Note (8): Uncertainties in V* are set to 17km/s (Section 2.1.3).
Note (9): For each galaxy, we assign the largest reliable velocity derived
from either gas or stellar kinematics as the characteristic internal
velocity V. See section 2.1.4.
Note (10): "ir", "nr", "sr", and "sd" indicate the origin of the final V
estimates from ionized-gas rotation Vpmm (79 galaxies), neutral gas
rotation W50 (53 galaxies), stellar rotation V* (12 galaxies), or
stellar dispersion (47 galaxies). See section 2.1.4.
Note (11): MHI are measured directly from 21cm fluxes using the equation:
MHI=1.4x2.36x105fHI(cz/H0)2M☉, which combines the
expression from Haynes & Giovanelli (1984AJ.....89..758H 1984AJ.....89..758H) with a 1.4x
correction factor for He (see section 2.1.2).
Note (12): Range of heliocentric velocities used in the HI flux measurement
or upper limit determination.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 27-Mar-2015