J/MNRAS/414/940 ATLAS3D project. IV. (Young+, 2011)
The ATLAS3D project. IV. The molecular gas content of early-type galaxies.
Young L.M., Bureau M., Davis T.A., Combes F., McDermid R.M., Alatalo K.,
Blitz L., Bois M., Bournaud F., Cappellari M., Davies R.L., de Zeeuw P.T.,
Emsellem E., Khochfar S., Krajnovic D., Kuntschner H., Lablanche P.-Y.,
Morganti R., Naab T., Oosterloo T., Sarzi M., Scott N., Serra P.,
Weijmans A.-M.
<Mon. Not. R. Astron. Soc. 414, 940 (2011)>
=2011MNRAS.414..940Y 2011MNRAS.414..940Y
ADC_Keywords: Surveys ; Galaxy catalogs ; Spectroscopy ; Carbon monoxide
Keywords: galaxies: elliptical and lenticular, cD - galaxies: evolution -
galaxies: ISM - galaxies: structure - radio lines: galaxies
Abstract:
We have carried out a survey for CO J=1-0 and J=2-1 emission in
the 260 early-type galaxies of the volume-limited ATLAS3D sample, with
the goal of connecting their star formation and assembly histories to
their cold gas content. This is the largest volume-limited CO survey
of its kind and is the first to include many Virgo cluster members.
Sample members are dynamically hot galaxies with a median stellar mass
∼3x1010M☉; they are selected by their morphology rather than
colour, and the bulk of them lie on the red sequence. The overall CO
detection rate is 56/259=0.22±0.03, with no dependence on the K
luminosity and only a modest dependence on the dynamical mass. There
are a dozen CO detections among the Virgo cluster members; statistical
analysis of their H2 mass distributions and their dynamical status
within the cluster shows that the cluster's influence on their
molecular masses is subtle at best, even though (unlike spirals) they
seem to be virialized within the cluster. We suggest that the cluster
members have retained their molecular gas through several Gyr
residences in the cluster.
Description:
The IRAM 30-m telescope at Pico Veleta, Spain, was used for
simultaneous observations of the 12CO(1-0) and (2-1) emission
during 2007 July, 2008 March and 2008 November.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 88 272 CO intensities and H2 masses
table2.dat 102 55 Fitted properties of detected lines
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See also:
J/MNRAS/413/813 : ATLAS3D project. I. (Cappellari+, 2011)
J/MNRAS/414/888 : ATLAS3D project. III. (Emsellem+, 2011)
J/MNRAS/416/1680 : ATLAS3D project. VII (Cappellari+, 2011)
J/MNRAS/433/2812 : ATLAS3D project. XXIII (Krajnovic+, 2013)
J/MNRAS/446/120 : ATLAS3D project. XXIX (Duc+, 2015)
J/MNRAS/448/3484 : ATLAS3D Project. XXX (McDermid+, 2015)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1 A1 --- n_Gal [O] O: Observed, but not member of the
ATLAS3D sample
3- 12 A10 --- Gal Galaxy name
14- 17 F4.2 mK rms(1-0) ?=- rms noise level at CO(1-0) (1)
19- 23 F5.2 mK rms(2-1) ?=- rms noise level at CO(2-1) (1)
25- 30 F6.1 km/s Vel1 ?=- Velocity range (2)
32- 37 F6.1 km/s Vel2 ?=- Velocity range (2)
39- 44 F6.3 K.km/s I(1-0) ?=- Intregrated intensity at CO(1-0), quoted
as main beam brightness temperature Tmb
46- 50 F5.3 K.km/s e_I(1-0) ?=- rms uncertainty on I(1-0)
52- 58 F7.3 K.km/s I(2-1) ?=- Intregrated intensity at CO(2-1), quoted
as main beam brightness temperature Tmb
60- 64 F5.3 K.km/s e_I(2-1) ?=- rms uncertainty on I(2-1)
66 A1 --- l_Ratio Limit flag on Ratio (3)
67- 70 F4.2 --- Ratio ?=- Intensity ratio CO(2-1)/CO(1-0)
72- 75 F4.2 --- e_Ratio ?=- rms uncertainty on Ratio
77 I1 --- Ref Data source (5)
79 A1 --- l_logMH2 Limit flag on logMH2 (3σ limit)
80- 83 F4.2 [Msun] logMH2 H2 mass (4)
85- 88 F4.2 [Msun] e_logMH2 ? rms uncertainty on logMH2
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Note (1): The rms noise values are for channels binned to 31km/s.
Note (2): The velocity range is either 300km/s (for non-detections) or the
actual range used in the sums (for detections).
Note (3): Where the line ratio is a limit, it is computed using the
3σ upper limit on the undetected line.
Note (4): H2 masses assume the distances listed in Paper I (Cappellari et al.,
2011, Cat. J/MNRAS/413/813). For galaxies taken from the literature,
we give only the H2 mass corrected to our assumed distance and other
quantities may be found in the original sources.
Note (5): Data sources as follows:
1 = this paper
2 = Combes et al. (2007MNRAS.377.1795C 2007MNRAS.377.1795C)
3 = Welch & Sage (2003ApJ...584..260W 2003ApJ...584..260W)
4 = Sage et al. (2007ApJ...657..232S 2007ApJ...657..232S)
5 = Wiklind et al. (1995A&A...297..643W 1995A&A...297..643W)
6 = Young (2002AJ....124..788Y 2002AJ....124..788Y)
7 = Welch et al. (2010ApJ...725..100W 2010ApJ...725..100W)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- n_Gal [O] O: Observed, but not members of the
ATLAS3D sample
3- 12 A10 --- Gal Galaxy name
14- 18 F5.2 K.km/s I(1-0) ?=- Line area in CO(1-0)
20- 23 F4.2 K.km/s e_I(1-0) ?=- rms uncertainty on I(1-0)
25- 29 F5.2 K.km/s I(2-1) ?=- Line area in CO(2-1)
31- 34 F4.2 K.km/s e_I(2-1) ?=- rms uncertainty on I(2-1)
36- 41 F6.1 km/s V(1-0) ?=- Central velocity in CO(1-0)
43- 46 F4.1 km/s e_V(1-0) ?=- rms uncertainty on V(1-0)
48- 53 F6.1 km/s V(2-1) ?=- Central velocity in CO(2-1)
55- 58 F4.1 km/s e_V(2-1) ?=- rms uncertainty on V(2-1)
60- 64 F5.1 km/s DV(1-0) ?=- FWHM in CO(1-0)
66- 69 F4.1 km/s e_DV(1-0) ?=- rms uncertainty on DV(1-0)
71- 75 F5.1 km/s DV(2-1) ?=- FWHM in CO(2-1)
77- 80 F4.1 km/s e_DV(2-1) ?=- rms uncertainty on DV(2-1)
82- 86 F5.1 mK Tmb(1-0) ?=- Peak brightness temperature in CO(1-0)
88- 92 F5.1 mK Tmb(2-1) ?=- Peak brightness temperature in CO(2-1)
94-102 A9 --- Com Comments (1)
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Note (1): Comments as follows:
a = line profile is notably asymmetric
a* = line is sufficiently asymmetric that the peak brightness
temperature (and area, systemic velocity and width for NGC 3665
in 2-1) has been measured directly off the profile rather than
with a fit.
2h = double-horned line profile
2h? = possibly double-horned line profile
Notes on specific galaxies:
* NGC 1266: the 1-0 line is, formally speaking, adequately fitted with one
Gaussian component but the 2-1 line has broad, low-level wings which
require two Gaussian components of the same centre and different widths
* NGC 6014: the line profile is neither a double horn nor a Gaussian, but
the central dip suggests a ringlike CO distribution
* NGC 4281, 5638 and 7454: the spectrum shows hints of two peaks. The peaks
were fitted independently and both velocities are listed. Formally, the
Gaussian fit detects each of these with an integrated area greater than
3σ, but as there is no emission within 300km/s of the optical
velocity it is a non-detection in Table 1 and it is NOT counted as a
detection in the rest of the analysis.
* NGC 4643 is formally detected via the integrated intensity in the central
300km/s of the 2-1 spectrum and its line is also suggestive of two
peaks. As for NGC 4281, the two velocities listed are those of the two
peaks (rather than the systemic velocity that one would infer from
assuming that those are double horned).
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History:
From electronic version of the journal
References:
Cappellari et al., Paper I 2011MNRAS.413..813C 2011MNRAS.413..813C, Cat. J/MNRAS/413/813
Krajnovic et al., Paper II 2011MNRAS.414.2923K 2011MNRAS.414.2923K
Emsellem et al., Paper III 2011MNRAS.414..888E 2011MNRAS.414..888E, Cat. J/MNRAS/414/888
Davis et al., Paper V 2011MNRAS.414..968D 2011MNRAS.414..968D
Bois et al., Paper VI 2011MNRAS.416.1654B 2011MNRAS.416.1654B
Cappellari et al., Paper VII 2011MNRAS.416.1680C 2011MNRAS.416.1680C, Cat. J/MNRAS/416/1680
Khochfar et al., Paper VIII 2011MNRAS.417..845K 2011MNRAS.417..845K
Duc et al., Paper IX 2011MNRAS.417..863D 2011MNRAS.417..863D
Davis et al., Paper X 2011MNRAS.417..882D 2011MNRAS.417..882D
Crocker et al., Paper XI 2012MNRAS.421.1298C 2012MNRAS.421.1298C
Lablanche et al., Paper XII 2012MNRAS.424.1495L 2012MNRAS.424.1495L
Serra et al., Paper XIII 2012MNRAS.422.1835S 2012MNRAS.422.1835S
Krajnovic et al., Paper XIV 2013MNRAS.432.1768K 2013MNRAS.432.1768K
Cappellari et al., Paper XV 2013MNRAS.432.1709C 2013MNRAS.432.1709C
Bayet et al., Paper XVI 2013MNRAS.432.1742B 2013MNRAS.432.1742B
Krajnovic et al., Paper XVII 2013MNRAS.432.1768K 2013MNRAS.432.1768K
Alatalo et al., Paper XVIII 2013MNRAS.432.1796A 2013MNRAS.432.1796A
Sarzi et al., Paper XIX 2013MNRAS.432.1845S 2013MNRAS.432.1845S
Cappellari et al., Paper XX 2013MNRAS.432.1862C 2013MNRAS.432.1862C
Scott et al., Paper XXI 2013MNRAS.432.1894S 2013MNRAS.432.1894S
Martig et al., Paper XXII 2013MNRAS.432.1914M 2013MNRAS.432.1914M
Krajnovic et al., Paper XXIII 2013MNRAS.433.2812K 2013MNRAS.433.2812K, Cat. J/MNRAS/433/2812
Davis et al., Paper XXIV 2013MNRAS.429..534D 2013MNRAS.429..534D
Cappellari et al., Paper XXV 2013MNRAS.432.1709C 2013MNRAS.432.1709C
Bayet et al., Paper XXVI 2013MNRAS.432.1742B 2013MNRAS.432.1742B
Krajnovic et al., Paper XXVII 2013MNRAS.432.1768K 2013MNRAS.432.1768K
Alatalo et al., Paper XXVIII 2013MNRAS.432.1796A 2013MNRAS.432.1796A
Duc et al., Paper XXIX 2015MNRAS.446..120D 2015MNRAS.446..120D
McDermid et al., Paper XXX 2015MNRAS.448.3484M 2015MNRAS.448.3484M, Cat. J/MNRAS/448/3484
(End) Patricia Vannier [CDS] 23-Jan-2012