M 31's Molecular Arms at All Scales to Below 10 pc

Neininger, N.; Nieten, Ch.; Guèlin, M.; Ungerechts, H.; Lucas, R.; Müller, S.; Wielebinski, R.

doi:10.1017/s0074180900221451

Cited by 16 publications

(30 citation statements)

References 5 publications

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“…In regions with CO emission, the excess dust emission with respect to this ratio indicates the mass of H 2 . This technique has been succesfully applied to M 51, NGC 891, NGC 4565 and to some nearby irregular galaxies such as the Magellanic Clouds (Guélin et al 1995;Guélin et al 1993;Neininger et al 1996;Israel 1997).…”

Section: An Alternative Methodsmentioning

confidence: 99%

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Molecular gas in normal late-type galaxies

Boselli

Lequeux²,

Gavazzi³

2002

A&A

219

390

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Abstract. We present 12 CO(J = 1-0) line observations of 22 low-luminosity spiral galaxies in the Virgo cluster. These data, together with 244 others available in the literature, allow us to build a large sample that we use to study the molecular gas properties of galaxies spanning a large range of morphological types and luminosities and belonging to different environments (clusters -field). The molecular gas content of the target galaxies is estimated using a luminosity-dependent X = N(H2)/I(CO) conversion factor that has been calibrated on a sample of nearby galaxies. X spans from ∼10 20 mol cm −2 (K km s −1 ) −1 in giant spirals to ∼10 21 mol cm −2 (K km s −1 ) −1 in dwarf irregulars. The value of the X conversion factor is found consistent with a value derived independently from dust masses estimated from FIR fluxes, with a metallicity-dependent dust to gas ratio. The relationships between X and the UV radiation field (as traced by the Hα + [NII]EW), the metallicity and the H band luminosity are analysed. We show that the molecular gas contained in molecular clouds or complexes is of the order of 15% of the total gas on average whatever the luminosity or the Hubble type of the galaxies. We discuss the relation between the star formation rate and the molecular gas content and estimate the average star formation efficiency of late-type galaxies.

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Section: An Alternative Methodsmentioning

confidence: 99%

“…The technique applied by Guélin and collaborators to a few nearby galaxies (Guélin et al 1993(Guélin et al , 1995Neininger et al 1996; see also Israel 1997) seems very promising. It consists of determining the amount of dust from millimetric/submillimetric observations and correlating it with CO and HI.…”

Section: Introductionmentioning

confidence: 99%

Molecular gas in normal late-type galaxies

Boselli

Lequeux²,

Gavazzi³

2002

A&A

219

390

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“…The strong submillimeter emission found in all the observed galaxies could not be accounted for by dust emitting at a uniform temperature, and the far-infrared (FIR) spectra were interpreted in terms of two dust components of about 16 and 53 K. This interpretation suggested that the peak of the FIR emission should be at wavelengths between 100 and 200 km. Subsequent submillimeter observations done with the 30 m IRAM (Pico Veleta) telescope also suggested the presence of a cold dust component in individual nearby galaxies : NGC 891 et al 1993), NGC 3627 (Guelin (Sievers et al 1994), NGC 4631 (Braine et al 1995), M51 et al 1995), NGC 4565 (Neininger et al 1996), NGC (Guelin 3079 , and NGC 5907 . The enhanced sensitivity and overall efficiency improvement of the Submillimeter Common-User Bolometric Array on the James Clerk Maxwell Telescope extended our knowledge of the quantity of cold dust by probing both more "" quiescent ÏÏ galaxies and also by mapping its distribution with higher resolution (Alton et al 1998a(Alton et al , 2001Israel, Van Der Werf, & Tilanus 1999 ;Bianchi et al 2000b).…”

Section: Introductionmentioning

confidence: 94%

Cold Dust in Late‐Type Virgo Cluster Galaxies

Popescu¹,

Tuffs²,

Voêlk³

et al. 2002

ApJ

133

144

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We have statistically analyzed the spatially integrated far-infrared (FIR) emissions of the complete volume-and luminosity-limited sample of late-type (later than S0) Virgo Cluster galaxies measured using the Infrared Space Observatory by Tu †s and coworkers in bands centered on 60, 100, and 170 km. Thirty of 38 galaxies detected at all three wavelengths contain a cold dust emission component, present within all morphological types of late-type systems ranging from early giant spiral galaxies to blue compact dwarfs (BCDs) and which could not have been recognized by IRAS. We Ðtted the data with a superposition of two modiÐed blackbody functions, physically identiÐed with a localized warm dust emission component associated with H II regions (whose temperature was constrained to be 47 K), and a di †use emission component of cold dust. The cold dust temperatures were found to be broadly distributed, with a median of 18 K, some 8È10 K lower than would have been predicted from IRAS. The derived total dust mass is correspondingly increased by factors of typically 6È13. A good linear correlation is found between the "" warm FIR ÏÏ luminosities and the Ha equivalent widths (EWs), supporting the assumptions of our constrained spectral energy distribution Ðt procedure. We also found a good nonlinear correlation between the "" cold FIR ÏÏ luminosities and the Ha EWs, consistent with the prediction of Popescu and coworkers that the FIR-submillimeter emission should mainly be due to di †use nonionizing UV photons. Both the "" warm ÏÏ and the "" cold ÏÏ FIR luminosity components are nonlinearly correlated with the (predominantly nonthermal) radio luminosities. There is a tendency for the temperatures of the cold dust component to become colder and for the cold dust surface densities (normalized to optical area) to increase for later morphological types. A particularly signiÐcant result concerns the low dust temperatures (ranging down to less than 10 K) and large dust masses associated with the Im and BCD galaxies in our sample. We propose two scenarios to account for the FIR characteristics of these systems.

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“…To these, we can add 71 galaxies observed along the major axis during the FCRAO CO survey of nearby galaxies by Young et al (1995). Another object, NGC 4565, has also been partly mapped with the IRAM 30 m (Neininger et al 1996) and with the 45 m Nobeyama (Sofue & Nakai 1994) radiotelescopes. Because of the complete coverage of the stellar disc, in particular for the single-dish observations done at the Nobeyama, IRAM, and FCRAO radio telescopes, we consider that all these data are of much higher quality than other singlebeam observations that require aperture corrections.…”

Section: Total Co Fluxesmentioning

confidence: 99%

“…We thus end up with 37 HRS galaxies with integrated data, 17 from Kuno et al (2007), 0 from Helfer et al (2003) 4 , 6 from Chung et al (2009a), and 13 from Young et al (1995). To these we can add a galaxy, NGC 4565 (HRS 213), partly mapped by Neininger et al (1996) with the IRAM radiotelescope and by Sofue & Nakai (1994) with the Nobeyama radiotelescope. By correcting their own independent sets of data to extend the measure of the CO flux to the whole galaxy, they end up with a total flux of SCO = 1672.2 Jy km s −1 and SCO = 1643 Jy km s −1 , respectively.…”

Section: Data Ismentioning

confidence: 99%

Cold gas properties of theHerschelReference Survey

Boselli

Cortese

Boquien

2014

A&A

149

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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M 31's Molecular Arms at All Scales to Below 10 pc

Cited by 16 publications

References 5 publications

Molecular gas in normal late-type galaxies

Molecular gas in normal late-type galaxies

Cold Dust in Late‐Type Virgo Cluster Galaxies

Cold gas properties of theHerschelReference Survey

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