Molecules in galaxies. III - The Virgo cluster

Stark, A. A.; Knapp, G. R.; Bally, John; Wilson, R. W.; Penzias, A. A.; Rowe, Harrison E.

doi:10.1086/164717

Cited by 86 publications

(78 citation statements)

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“…Overall, there is a quite good agreement with previous observations. The only exception is NGC 4388 for which Stark et al (1986) reported M H 2 = 2.2 × 10 9 M , a value ∼30% higher than our estimate. The beam size of their telescope is larger, 100 , and they observed the disk in 5 different positions, with an offset of 1.…”

Section: Ngc 4294 Ngc 4351 and Ngc 4424contrasting

confidence: 89%

“…Our map does not extend farther than 80 along the disk; however the emission decreases steeply already at ∼30-40 from the center. Our molecular mass estimate agrees with the value of Kenney & Young (1986) which have sampled similar regions of this galaxy as Stark et al (1986), but with a smaller beam. Cortés et al (2006) carried out interferometric observations of the 12 CO(1-0) emission line of the central regions of NGC 4424, and found a molecular gas mass of 1.6 × 10 8 M .…”

Section: Ngc 4294 Ngc 4351 and Ngc 4424supporting

confidence: 88%

“…For NGC 4351 and NGC 4294 we found the lowest H 2 masses of the observed sample, 7.1 ×10 7 M , and 7.3 ×10 7 M , and also low molecular fractions, f mol = 0.17, and 0.04, respectively. For NGC 4424 we found a M H 2 = 4.2 × 10 8 M , with a molecular A75, page 9 of 17 Figure 10 shows the comparison of our measurement of the molecular gas mass with previous estimates (Stark et al 1986;Young et al 1995;Boselli et al 1995b;Smith & Madden 1997;Chung et al 2009b). We have rescaled the literature values to match our choice of X CO and distance.…”

Section: Ngc 4294 Ngc 4351 and Ngc 4424mentioning

confidence: 60%

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TheHerschelVirgo Cluster Survey

Pappalardo

Bianchi

Corbelli

et al. 2012

A&A

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Aims. We investigate the dust-to-gas mass ratio and the environmental effects on the various components of the interstellar medium for a spatially resolved sample of Virgo spirals. Methods. We have used the IRAM-30 m telescope to map over their full extent NGC 4189, NGC 4298, NGC 4388, and NGC 4299 in the 12 CO(1-0) and the 12 CO(2-1) lines. We observed the same lines in selected regions of NGC 4351, NGC 4294, and NGC 4424. The CO observations are combined with Herschel maps in 5 bands between 100-500 μm from the HeViCS survey, and with HI data from the VIVA survey, to obtain spatially resolved dust and gas distributions. We studied the environmental dependencies by adding to our sample eight galaxies with 12 CO(1-0) maps from the literature. Results. We estimate the integrated mass of molecular hydrogen for the galaxies observed in the CO lines. We find molecular-to-total gas mass fractions between 0.04 ≤ f mol ≤ 0.65, with the lowest values for the dimmest galaxy in the B-band. The integrated dust-togas ratio ranges between 0.011 and 0.004. For the 12 mapped galaxies we derive the radial distributions of the atomic gas, molecular gas, and dust. We also study the effect of different CO-to-H 2 conversion factors. Both the molecular gas and the dust distributions show steeper radial profiles for HI-deficient galaxies and the average dust-to-gas ratio for these galaxies increases or stays radially constant. On scales of ∼3 kpc, we find a strong correlation between the molecular gas and the 250 μm surface brightness that is tighter than average for non-deficient galaxies. The correlation becomes linear if we consider the total gas surface mass density. However, the inclusion of atomic hydrogen does not improve the statistical significance of the correlation. Conclusions. The environment can modify the distributions of molecules and dust within a galaxy, although these components are more tightly bound than the atomic gas.

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Section: Ngc 4294 Ngc 4351 and Ngc 4424contrasting

confidence: 89%

Section: Ngc 4294 Ngc 4351 and Ngc 4424supporting

confidence: 88%

Section: Ngc 4294 Ngc 4351 and Ngc 4424mentioning

confidence: 60%

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TheHerschelVirgo Cluster Survey

Pappalardo

Bianchi

Corbelli

et al. 2012

A&A

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“…(6); right panels) on logarithmic (upper panels) and linear (in the range 0-5000 Jy km s −1 sampled by the HRS galaxies) scales (lower panels) for galaxies with integrated data from Kuno et al (2007). Different symbols are used for galaxies observed in the FCRAO survey of Young et al (1995;cyan), Stark et al (1986;magenta), and other references (black). Filled dots are for galaxies with D 25 (B)/θ ≤ 5, empty symbols for those objects with D 25 (B)/θ > 5.…”

Section: Extrapolation Of the Central Beammentioning

confidence: 99%

“…Relationship between the ratio of the total CO flux as determined from the extrapolation of the central beam observation to the total value determined from the maps for galaxies with integrated data from Kuno et al (2007) as a function of the filling factor ff, defined as the fraction of the galaxy covered by the central beam (lower panel). Different symbols are used for the galaxies observed in the FCRAO survey of Young et al (1995;cyan), Stark et al (1986;magenta) and other references (black). Filled dots are for galaxies with D 25 (B)/θ ≤ 5, empty symbols for those objects with D 25 (B)/θ > 5.…”

Section: Multiple Beam Observationsmentioning

confidence: 99%

Cold gas properties of theHerschelReference Survey

Boselli

Cortese

Boquien

2014

A&A

148

257

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We present new 12 CO(1-0) observations of 59 late-type galaxies belonging to the Herschel Reference Survey (HRS), a complete K-band-selected, volume-limited (15 D 25 Mpc) sample of nearby galaxies spanning a wide range in morphological type and luminosity. We studied different recipes to correct single-beam observations of nearby galaxies of different sizes and inclinations for aperture effects. This was done by comparing single-beam and multiple-beam observations along the major axis, which were corrected for aperture effects using different empirical or analytical prescriptions, to integrated maps of several nearby galaxies, including edge-on systems observed by different surveys. The resulting recipe is an analytical function determined by assuming that late-type galaxies are 3D exponentially declining discs with a characteristic scale length r CO = 0.2 r 24.5 , where r 24.5 is the optical, g-(or B-) band isophotal radius at the 24.5 mag arcsec −2 (25 mag arcsec −2 ), as well as a scale height z CO = 1/100 r 24.5 . Our new CO data are then combined with those available in the literature to produce the most updated catalogue of CO observations for the HRS, now including 225 out of the 322 galaxies of the complete sample. The 3D exponential disc integration is applied to all the galaxies of the sample to measure their total CO fluxes, which are later transformed into molecular gas masses using a constant and a luminosity-dependent X CO conversion factor. We also collect Hi data for 315 HRS galaxies from the literature and present it in a homogenised form.

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References for 9.2

Huchtmeier¹

Interstellar Matter, Galaxy, Universe

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Molecules in galaxies. III - The Virgo cluster

Cited by 86 publications

References 0 publications

TheHerschelVirgo Cluster Survey

TheHerschelVirgo Cluster Survey

Cold gas properties of theHerschelReference Survey

References for 9.2

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