<sup>12</sup>
                    CO(
                    <i>J</i>
                    = 1 – 0) ON-THE-FLY MAPPING SURVEY OF THE VIRGO CLUSTER SPIRALS. I. DATA AND ATLAS

Chung, Eun Jung; Rhee, Myung-Hyun; Kim, Hyo-Ryoung; Yun, Min S.; Young, J. S.

doi:10.1088/0067-0049/184/2/199

Cited by 36 publications

(55 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…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%

TheHerschelVirgo Cluster Survey

Pappalardo

Bianchi

Corbelli

et al. 2012

A&A

View full text Add to dashboard Cite

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.

show abstract

Section: Ngc 4294 Ngc 4351 and Ngc 4424mentioning

confidence: 60%

TheHerschelVirgo Cluster Survey

Pappalardo

Bianchi

Corbelli

et al. 2012

A&A

View full text Add to dashboard Cite

show abstract

“…Of these, 18 objects have been observed by Kuno et al (2007) with the 25 beams BEARS array mounted on the 45 m Nobeyama Radio Observatory telescope, 19 objects by Chung et al (2009a) with the 16 beams SEQUOIA array on the 13.7 m FCRAO radio telescope, and 2 other galaxies with the IRAM 30 m radio telescope by our team (see below). Ten galaxies have also been observed during the BIMA SONG survey of nearby galaxies with the Owens Valley Radio Observatory in interferometric mode by Helfer et al (2003).…”

Section: Total Co Fluxesmentioning

confidence: 91%

“…The linear best fit to the data, determined assuming the Kuno et al (2007) data as independent variable in the range 100-5000 Jy km s −1 , are shown by the red dotted line (Helfer et al 2003), the blue long dashed line (Chung et al 2009a) and the cyan solid line (Young et al 1995). The short dashed black line shows the 1:1 relationships.…”

Section: Figmentioning

confidence: 95%

“…Comparison between the integrated SCO fluxes determined by Kuno et al (2007) and those determined by Helfer et al (2003; red filled dots), Chung et al (2009a; blue filled triangles), our own observations of the two galaxies NGC 4548 and NGC 4579 with the IRAM radiotelescope (green filled squares) and the extrapolated fluxes of the FCRAO survey (Young et al 1995; cyan empty circles) on logarithmic scale for all galaxies in common (left) and on linear scale for those objects with SCO in the range 100-5000 Jy km s −1 sampled by the HRS (right). The linear best fit to the data, determined assuming the Kuno et al (2007) data as independent variable in the range 100-5000 Jy km s −1 , are shown by the red dotted line (Helfer et al 2003), the blue long dashed line (Chung et al 2009a) and the cyan solid line (Young et al 1995).…”

Section: Figmentioning

confidence: 95%

See 1 more Smart Citation

Cold gas properties of theHerschelReference Survey

Boselli

Cortese

Boquien

2014

A&A

148

257

View full text Add to dashboard Cite

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.

show abstract

“…7 the relationship between the ratio of the atomic and molecular gas-to-stellar (i-band) isophotal diameter ratio and the Hi-deficiency parameter. CO and Hi isophotal diameters are taken from the subsample of HRS galaxies mapped by Chung et al (2009b) 3 in CO and by Chung et al (2009a) in Hi. Both molecular and atomic gas isophotal diameters are determined where the gas column density drops to 1 M pc −2 .…”

Section: Ram Pressure Strippingmentioning

confidence: 99%

Cold gas properties of theHerschelReference Survey

Boselli

Cortese

Boquien

et al. 2014

A&A

176

250

View full text Add to dashboard Cite

The Herschel Reference Survey is a complete volume-limited, K-band-selected sample of nearby objects including Virgo cluster and isolated objects. Using a recent compilation of Hi and CO data for this sample we study the effects of the cluster environment on the molecular gas content of spiral galaxies. With the subsample of unperturbed field galaxies, we first identify the stellar mass as the scaling variable that traces the total molecular gas mass of galaxies better. We show that, on average, Hi-deficient galaxies are significantly offset (4σ) from the M(H 2 ) vs. M star relation for Hi-normal galaxies. We use the M(H 2 ) vs. M star scaling relation to define the H 2 -deficiency parameter as the difference, on logarithmic scale, between the expected and observed molecular gas mass for a galaxy of given stellar mass. The H 2 -deficiency parameter shows a weak and scattered relation with the Hi-deficiency parameter, here taken as a proxy for galaxy interactions with the surrounding cluster environment. We also show that, as for the atomic gas, the extent of the molecular disc decreases with increasing Hi-deficiency. All together, these results show that cluster galaxies have, on average, a lower molecular gas content than similar objects in the field. Our analysis indicates that ram pressure stripping is the physical process responsible for this molecular gas deficiency. The slope of the H 2 − de f vs. Hi − de f relation is less than unity, while the D(Hi)/D(i) vs. Hi − de f relation is steeper than the D(CO)/D(i) vs. Hi − de f relation, thereby indicating that the molecular gas is removed less efficiently than the atomic gas. This result can be understood if the atomic gas is distributed on a relatively flat disc that is more extended than the stellar disc. It is thus less anchored to the gravitational potential well of the galaxy than the molecular gas phase, which is distributed on an exponential disc with a scalelength r CO 0.2r 24.5 (g). There is a clear trend between the NUV-i colour index, which is a proxy for the specific star formation activity, and the H 2 -deficiency parameter, which suggests that molecular gas removal quenches the activity of star formation. This causes galaxies migrate from the blue cloud to the green valley and, eventually, to the red sequence. The total gas-consumption timescale of gas deficient cluster galaxies is comparable to that of isolated, unperturbed systems. The total gas depletion timescale determined by considering the recycled fraction is τ gas,R 3.0−3.3 Gyr, which is significantly larger than the typical timescale for total gas removal in a ram pressure stripping process, indicated by recent hydrodynamical simulations to be τ RP 1.5 Gyr. The comparison of these timescales suggests that ram pressure, rather than a simple stop of the infall of pristine gas from the halo, will be the dominant process driving the future evolution of these cluster galaxies.

show abstract

¹² CO( J = 1 – 0) ON-THE-FLY MAPPING SURVEY OF THE VIRGO CLUSTER SPIRALS. I. DATA AND ATLAS

Cited by 36 publications

References 32 publications

TheHerschelVirgo Cluster Survey

TheHerschelVirgo Cluster Survey

Cold gas properties of theHerschelReference Survey

Cold gas properties of theHerschelReference Survey

Contact Info

Product

Resources

About

12 CO( J = 1 – 0) ON-THE-FLY MAPPING SURVEY OF THE VIRGO CLUSTER SPIRALS. I. DATA AND ATLAS

Cited by 36 publications

References 32 publications

TheHerschelVirgo Cluster Survey

TheHerschelVirgo Cluster Survey

Cold gas properties of theHerschelReference Survey

Cold gas properties of theHerschelReference Survey

Contact Info

Product

Resources

About

¹² CO( J = 1 – 0) ON-THE-FLY MAPPING SURVEY OF THE VIRGO CLUSTER SPIRALS. I. DATA AND ATLAS