J/A+A/540/A96 Molecular gas in Hickson Compact Groups (Martinez-Badenes+, 2012)
Molecular gas content and SFR in Hickson Compact Groups: enhanced or deficient?
Martinez-Badenes V. Lisenfeld U., Espada D., Verdes-Montenegro L.,
Garcia-Burillo S., Leon S., Sulentic J., Min Y.S.
<Astron. Astrophys. 540, A96 (2012)>
=2012A&A...540A..96M 2012A&A...540A..96M
ADC_Keywords: Clusters, galaxy ; Carbon monoxide ; H I data ; Infrared sources
Keywords: ISM: molecules - galaxies: evolution - galaxies: ISM -
galaxies: interactions - galaxies: star formation -
galaxies: groups: general
Abstract:
We study the effect of the extreme environment in Hickson Compact
Groups (HCGs) on the molecular gas mass, MH2, and the star
formation rate (SFR) of galaxies as a function of atomic hydrogen (HI)
content and evolutionary phase of the group.
We selected a redshift-limited (D<100Mpc) sample of 88 galaxies in
20 HCGs with available atomic hydrogen (HI) VLA maps, covering a wide
range of HI deficiencies and evolutionary phases of the groups
containing at least one spiral galaxy. We observed the CO(1-0) and
CO(2-1) lines with the IRAM 30m telescope for 47 galaxies. Together
with literature data, our sample contains CO(1-0) spectra for 86
galaxies. We derived the far-infrared (FIR) luminosity LFIR from IRAS
data and used it as a tracer of the star formation rate (SFR). We
calculated the HI mass, MHI LFIR and MH2 deficiencies, based on
the values expected from LB and LK in isolated galaxies from the
AMIGA sample. We limited our statistical analysis to spiral galaxies,
since the large number of upper limits did not allow drawing strong
conclusions about MH2 and LFIR in early-type galaxies.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 56 87 General data for the sample
table2.dat 72 89 Observed and derived molecular gas properties
table3.dat 52 85 Far-infrared emission and star formation rate
table5.dat 26 87 Deficiencies derived from the blue luminosity
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See also:
VII/213 : Hickson's Compact groups of Galaxies (Hickson+ 1982-1994)
J/A+A/533/A142 : UV-to-IR fluxes of Hickson compact groups (Bitsakis+, 2011)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Name Galaxy designation (G1)
7- 10 I4 km/s HRV ?=- Heliocentric radial velocity in the
ratio definition
12- 14 I3 km/s sigma Velocity dispersion of the galaxies in the group
16- 19 F4.1 Mpc Dist Distance to the corresponding HCG (1)
21- 24 F4.1 --- MType ?=- Morphological type (2)
26- 29 F4.2 arcmin D25 ?=- Optical isophotal major diameter at the
isophotal level 25mag/arcsec2 taken from LEDA
31- 35 F5.2 mag BcT ? Apparent blue magnitude taken from LEDA (3)
37- 41 F5.2 [Lsun] log(LB) Decimal logarithm of the blue luminosity in
units of bolometric solar luminosity
43- 47 F5.2 [Lsun] log(LK) ?=- Decimal logarithm of the luminosity in the
Ks-band in units of the the solar luminosity
in the Ks-band (4)
49 A1 --- l_logMHI Limit flag on logMHI (5)
50- 54 F5.2 [Msun] logMHI ? Logarithm of the mass of the atomic hydrogen
for galaxies observed with the VLA using
different combinations of the C and D
configurations
56 A1 --- Note [*] Individual note (6)
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Note (1): derived from the mean heliocentric velocity of the group as D=V/H0,
assuming a value of H0=75km/s/Mpc. The mean velocity of the group is
calculated averaging the velocity of the individual galaxies.
Note (2): given in the RC3 numerical scale (de Vaucouleur et al., 1991,
Cat. VII/155).
Note (3): corrected for Galactic dust extinction, internal extinction and
K-correction
Note (4): calculated from the extrapolated magnitude in the Ks (2.17*10-6m)
band from the 2MASS Extended Source Catalog (Jarrett et al., 2000,
Cat. VII/233)
Note (5): Upper limit code for atomic gas mass as follows:
< = logMHI is an upper limit
> = logMHI is an upper limit (treated as a detection in the statistical
analysis
= logMHI is a detection
Note (6): The values of LB, LK and MHI for 31ac are the sum of their
respective values.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Name Galaxy designation (G1)
7 A1 --- l_ICO10 Limit flag on ICO10 (upper limit)
8- 12 F5.2 K.km/s ICO10 ?=- Velocity integrated intensity of the
CO(1-0) emission
14- 17 F4.2 K.km/s e_ICO10 ?=- Error of ICO10
20- 23 F4.2 mK rmsCO10 ?=- Root-mean-square noise of the CO(1-0)
spectrum
25 I1 --- r_ICO10 ?=- Reference of the CO(1-0) data (1)
27- 28 I2 arcsec beam ?=- Half power beam width of the telescope
for CO(1-0)
30- 32 I3 km/s dvCO10 ?=- Line width of the CO(1-0) emission
(if detected)
35 A1 --- l_ICO21 Limit flag on ICO21 (upper limit)
36- 40 F5.2 K.km/s ICO21 ?=- Velocity integrated intensity of the
CO(2-1) emission
42- 45 F4.2 K.km/s e_ICO21 ?=- Error of ICO21
47- 51 F5.2 mK rmsCO21 ?=- Root-mean-square noise of the CO(2-1)
spectrum
54- 56 I3 km/s dvCO21 ?=- Line width of the CO(2-1) emission
(if detected)
59 A1 --- l_log(MH2)o Limit flag on log(MH2)o (upper limit)
60- 63 F4.2 [Msun] log(MH2)o ?=- logarithm of the H2 mass, calculated
from the observed central ICO10
65 A1 --- l_log(MH2) Limit flag on log(MH2) (upper limit)
66- 70 F5.2 [Msun] log(MH2) ?=- logarithm of the H2 mass, extrapolated
to the emission from the total disk
72 A1 --- Note [*] Note (2)
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Note (1): Reference code for the ICO10 data as follows:
1 = our observations
2 = Leon et al. (1998A&A...330...37L 1998A&A...330...37L)
3 = Verdes-Montenegro et al. (1998ApJ...497...89V 1998ApJ...497...89V)
Note (2): The values of the observed and extrapolated MH2 for 31ac are the sum
of their respective values.
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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- 5 A5 --- Name Galaxy designation (G1)
7 I1 --- r_FIR Reference code for the FIR data (7)
9 A1 --- l_I60 Limit flag on I60 (upper limit)
10- 14 F5.2 Jy I60 IRAS flux at 60 micron, derived with
the tool SCANPI
16 A1 --- l_I100 Limit flag on I100 (upper limit)
17- 21 F5.2 Jy I100 IRAS flux at 100 micron, derived with
the tool SCANPI
23 A1 --- l_log(LFIR) Limit flag on log(LFIR) (upper limit)
24- 28 F5.2 [Lsun] log(LFIR) logarithm of the far-infrared luminosity
30 A1 --- l_SFR Limit flag on SFR (upper limit)
31- 35 F5.2 Msun/yr SFR Star formation rate,
derived from log(LFIR) (8)
37 A1 --- l_log(SFE) Limit flag on log(SFE)
(upper or lower limit)
38- 42 F5.2 [yr-1] log(SFE) ?=- Star formation efficiency, derived as
SFE=SFR/MH2
44 A1 --- l_log(sSFR) Limit flag on I60 (upper limit)
45- 50 F6.2 [Msun/yr] log(sSFR) ?=- Specific star formation rate, derived
as sSFR=SFR/Mstar, where Mstar is the
stellar mass derived from the luminosity
in the Ks band
52 A1 --- Note [*] Note (9)
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Note (7): Reference code for FIR data as follows:
1 = our data analysis
3 = from Verdes-Montenegro et al. (1998ApJ...497...89V 1998ApJ...497...89V)
Note (8): The value of the SFR is not displayed for galaxies with upper
limits in both LFIR and MH2.
Note (9): The SFE of 31ac has been calculated using the sum of their
respective MH2. The values of I60, I100, log(LFIR) of 37a, 37b, 37c
and 79a, 79b were corrected for blending on Spitzer 24 micron data
(see Sect. 3.2 of the paper for more details).
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Name Galaxy designation (G1)
7 A1 --- l_def(MH2) Limit flag on def(MH2) (lower limit)
8- 12 F5.2 [Msun] def(MH2) Deficiency of the H2 mass (10)
14 A1 --- l_def(LFIR) Limit flag on def(LFIR) (lower limit)
15- 19 F5.2 [Lsun] def(LFIR) ?=- Deficiency of the FIR luminosity (10)
21 A1 --- l_def(MHI) Limit flag on def(MHI) (lower or upper limit)
22- 26 F5.2 [Msun] def(MHI) ?=- Deficiency of the HI mass (10)
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Note (10): a deficiency in parameter X is defined as
def(X) = log(Xpredicted) - log(Xpbserved) ;
a negative deficiency implies therefore an excess
with respect to the predicted value.
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Global notes:
Note (G1): following the notation of Hickson (1982, Cat. VII/213)
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Acknowledgements:
Ute Lisenfeld, ute(at)ugr.es
(End) Ute Lisenfeld [UGR], Patricia Vannier [CDS] 12-Mar-2012