J/ApJ/733/L47 Galaxy bulge types within 11Mpc (Fisher+, 2011)
Demographics of bulge types within 11 Mpc and implications for galaxy evolution.
Fisher D.B., Drory N.
<Astrophys. J., 733, L47 (2011)>
=2011ApJ...733L..47F 2011ApJ...733L..47F
ADC_Keywords: Galaxy catalogs ; Morphology ; Galaxies, nearby
Keywords: galaxies: evolution - galaxies: fundamental parameters -
galaxies: general - galaxies: ISM - galaxies: photometry -
galaxies: spiral
Abstract:
We present an inventory of galaxy bulge types (elliptical galaxy,
classical bulge, pseudobulge, and bulgeless galaxy) in a
volume-limited sample within the local 11Mpc sphere using Spitzer
3.6um and Hubble Space Telescope data. We find that whether counting
by number, star formation rate, or stellar mass, the dominant galaxy
type in the local universe has pure disk characteristics (either
hosting a pseudobulge or being bulgeless). Galaxies that contain
either a pseudobulge or no bulge combine to account for over 80% of
the number of galaxies above a stellar mass of 109M☉.
Classical bulges and elliptical galaxies account for ∼1/4, and disks
for ∼3/4 of the stellar mass in the local 11Mpc. About 2/3 of all star
formation in the local volume takes place in galaxies with
pseudobulges. Looking at the fraction of galaxies with different bulge
types as a function of stellar mass, we find that the frequency of
classical bulges strongly increases with stellar mass, and comes to
dominate above 1010.5M☉. Galaxies with pseudobulges dominate
at 109.5-1010.5M☉. Yet lower-mass galaxies are most likely
to be bulgeless. If pseudobulges are not a product of mergers, then
the frequency of pseudobulges in the local universe poses a challenge
for galaxy evolution models.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 72 321 Sample data
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See also:
VII/155 : Third Reference Cat. of Bright Galaxies (RC3) (de Vaucouleurs+ 1991)
J/ApJS/196/11 : Bulge+disk decompositions of SDSS galaxies (Simard+, 2011)
J/ApJ/716/942 : Bulges of nearby galaxies with Spitzer (Fisher+, 2010)
J/ApJS/182/216 : Surface photometry of Virgo ellipticals (Kormendy+, 2009)
J/ApJ/706/599 : Hα and UV SFR in the local volume (Lee+, 2009)
J/ApJ/703/1672 : Far-IR and Hα fluxes in galaxies (Kennicutt+, 2009)
J/AJ/136/773 : Structure of classical bulges and pseudobulges (Fisher+, 2008)
J/ApJS/178/247 : Hα and [NII] survey in local 11 Mpc (Kennicutt+, 2008)
J/AJ/136/2782 : Star formation efficiency in nearby galaxies (Leroy+, 2008)
J/A+AS/145/405 : Box- and peanut-shaped bulges. I. (Luetticke+, 2000)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Galaxy name
16- 19 A4 --- Cat Bulge category (1)
21 A1 --- f_Cat [bcd] peculiarities on Cat (2)
23- 24 I2 --- T [-5/10]?=99 Galaxy Morphology type
26- 29 F4.1 Mpc Dist Distance (3)
31- 35 F5.1 mag BMag Absolute B-band magnitude (4)
37- 41 F5.2 [Msun] logM Log of total stellar mass
43- 47 F5.2 [Msun/yr] logSFR ? log of total star formation rate, logψ
49- 53 A5 --- Meth Star formation rate method (UV, 24 or Ha) (5)
55- 58 F4.2 --- B/T Bulge-to-total ratio
60- 62 F3.1 --- n ? Sersic index
64- 66 F3.1 --- e_n ? Uncertainty in n
68- 72 F5.2 [Msun/yr] log1kpc ? log of central 1kpc star formation rate
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Note (1): Category as follows:
E = Elliptical Galaxy;
C = Classical bulge;
P = Pseudobulge;
nb/d = no bulge/dwarf;
M = advanced stage merger
Note (2): Flag as follows:
b = NGC 5194 & NGC 5195 are currently interacting.
c = Categorized as classical bulge due to Sersic index despite
nuclear morphology.
d = Morphology strongly indicates pseudobulge, despite high Sersic index
Note (3): We adopt distances from Kennicutt et al. (2008, Cat. J/ApJS/178/247)
augmenting missing data from Tonry et al. (2001ApJ...546..681T 2001ApJ...546..681T),
Tully et al. (2009AJ....138..323T 2009AJ....138..323T), and Tully & Fisher
(1988cng..book.....T 1988cng..book.....T).
Note (4): We take BT values from de Vaucouleurs et al. (RC3, 1991,
Cat. VII/155) and HyperLEDA.
Note (5): Available means of measuring SFR in our sample include GALEX FUV
luminosity, Hα luminosity, and 24um dust emission; linear
combination of either Hα or UV (unobscured light) with 24um
(extincted light) is the most robust. See section 2 for further
explanations.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 19-Nov-2012