2011A&A...535A..13M


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.24CEST15:58:40

2011A&A...535A..13M - Astronomy and Astrophysics, volume 535A, 13-13 (2011/11-1)

The Herschel Virgo cluster survey. IX. Dust-to-gas mass ratio and metallicity gradients in four Virgo spiral galaxies.

MAGRINI L., BIANCHI S., CORBELLI E., CORTESE L., HUNT L., SMITH M., VLAHAKIS C., DAVIES J., BENDO G.J., BAES M., BOSELLI A., CLEMENS M., CASASOLA V., DE LOOZE I., FRITZ J., GIOVANARDI C., GROSSI M., HUGHES T., MADDEN S., PAPPALARDO C., POHLEN M., DI SEREGO ALIGHIERI S. and VERSTAPPEN J.

Abstract (from CDS):

Using Herschel data from the open time key project the Herschel Virgo Cluster Survey (HeViCS), we investigated the relationship between the metallicity gradients expressed by metal abundances in the gas phase as traced by the chemical composition of HII regions, and in the solid phase, as traced by the dust-to-gas mass ratio. We derived the radial gradient of the dust-to-gas mass ratio for all galaxies observed by HeViCS whose metallicity gradients are available in the literature. They are all late type Sbc galaxies, namely NGC 4254, NGC 4303, NGC 4321, and NGC 4501. We fitted PACS and SPIRE observations with a single-temperature modified blackbody, inferred the dust mass, and calculated two dimensional maps of the dust-to-gas mass ratio, with the total mass of gas from available HI and CO maps. HI moment-1 maps were used to derive the geometric parameters of the galaxies and extract the radial profiles. We examined different dependencies on metallicity of the CO-to-H2 conversion factor (XCO), used to transform the 12CO observations into the amount of molecular hydrogen. We found that in these galaxies the dust-to-gas mass ratio radial profile is extremely sensitive to choice of the XCO value, since the molecular gas is the dominant component in the inner parts. We found that for three galaxies of our sample, namely NGC 4254, NGC 4321, and NGC 4501, the slopes of the oxygen and of the dust-to-gas radial gradients agree up to ∼0.6-0.7R25 using XCO values in the range 1/3-1/2 Galactic XCO. For NGC 4303 a lower value of XCO∼0.1x1020 is necessary. We suggest that such low XCO values might be due to a metallicity dependence of XCO (from close to linear for NGC 4254, NGC 4321, and NGC 4501 to superlinear for NGC 4303), especially in the radial regions RG<0.6-0.7R25 where the molecular gas dominates. On the other hand, the outer regions, where the atomic gas component is dominant, are less affected by the choice of XCO, and thus we cannot put constraints on its value there.

Abstract Copyright:

Journal keyword(s): galaxies: spiral - galaxies: abundances - submillimeter: galaxies - galaxies: ISM - dust, extinction

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 11053 1
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9559 1
3 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5194 1
4 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14993 1
5 NGC 2403 AGN 07 36 51.396 +65 36 09.17 9.31 8.84 8.38 8.19   ~ 1627 1
6 M 81 Sy2 09 55 33.17306143 +69 03 55.0609270   7.89 6.94     ~ 3998 5
7 M 99 H2G 12 18 49.625 +14 24 59.36 10.45 10.44 9.87     ~ 776 2
8 M 61 Sy2 12 21 54.9275149050 +04 28 25.588335799 10.07 10.18 9.65     ~ 880 2
9 M 100 AGN 12 22 54.9318850854 +15 49 20.294302163 10.04 10.05 9.35     ~ 1670 2
10 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5909 0
11 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6283 3
12 M 88 Sy2 12 31 59.216 +14 25 13.48   14.33 13.18     ~ 736 1
13 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 3834 4
14 M 10 GlC 16 57 09.05 -04 06 01.1     4.98     ~ 690 0

    Equat.    Gal    SGal    Ecl

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2020.10.24-15:58:40

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