Erratum: “Far‐Infrared Photometry of a Statistical Sample of Late‐Type Virgo Cluster Galaxies” (ApJS, 139, 37 [2002])

Tuffs, R.; Popescu, Cristina; Pierini, D.; Völk, H. J.; Hippelein, H.; Leech, K.; Metcalfe, L.; Heinrichsen, I.; Xu, C. K.

doi:10.1086/342485

Cited by 58 publications

(93 citation statements)

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“…IRAS beams are messy, so this is not the best way, but, for 10 of the galaxies listed in Table 1 and detected in the [C II] line emission (i.e. NGC 4178,4192,4293,4394,4429,4438,4450,4491,4569 and 4579), high signal-to-noise strip maps exist at 60 and 100 µm, obtained by Tuffs et al (2002) with the 40 arcsec HPBW instrument ISOPHOT (Lemke et al 1996). Tuffs et al have extracted the ISOPHOT far-IR photometry by fitting a model of the far-IR surface brightness distribution to the data.…”

Section: Discussionmentioning

confidence: 99%

[C II] emission and star formation in late-type galaxies

Pierini

Leech

Völk

2003

A&A

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Abstract. We study the relationship between gas cooling via the [C II] (λ = 158 µm) line emission and dust cooling via the far-IR continuum emission on the global scale of a galaxy in normal (i.e. non-AGN dominated and non-starburst) late-type systems. It is known that the luminosity ratio of total gas and dust cooling, L C II /L FIR , shows a non-linear behaviour with the equivalent width of the Hα (λ = 6563 Å) line emission, the ratio decreasing in galaxies of lower massive star-formation activity. This result holds despite the fact that known individual Galactic and extragalactic sources of the [C II] line emission show different [C II] line-to-far-IR continuum emission ratios. This non-linear behaviour is reproduced by a simple quantitative theoretical model of gas and dust heating from different stellar populations, assuming that the photoelectric effect on dust, induced by far-UV photons, is the dominant mechanism of gas heating in the general diffuse interstellar medium of the galaxies under investigation. According to the model, the global L C II /L FIR provides a direct measure of the fractional amount of non-ionizing UV light in the interstellar radiation field and not of the efficiency of the photoelectric heating. The theory also defines a method to constrain the stellar initial mass function from measurements of L C II and L FIR . A sample of 20 Virgo cluster galaxies observed in the [C II] line with the Long Wavelength Spectrometer on board the Infrared Space Observatory is used to illustrate the model. The limited statistics and the necessary assumptions behind the determination of the global [C II] luminosities from the spatially limited data do not allow us to establish definitive conclusions but data-sets available in the future will allow tests of both the reliability of the assumptions behind our model and the statistical significance of our results.

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Section: Discussionmentioning

confidence: 99%

[C II] emission and star formation in late-type galaxies

Pierini

Leech

Völk

2003

A&A

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“…In the Small Magellanic Cloud, IRAS observations suggested much more H 2 than seen from CO (Israel 1997;Leroy et al 2007a) and, thus, that CO may be underabundant or absent in regions where H 2 survives because the H 2 self-shields while the CO is photodissociated (e.g., Maloney & Black 1988). From ISO observations Tuffs et al (2002) obtained 3σ upper limits on 60 µm, 100 µm, and 170 µm FIR dust emission of IC3418 of < 0.04 Jy, < 0.03 Jy, and < 0.07 Jy, respectively. The total dust mass can be determined to within a factor of 3 from (e.g., Boselli et al 2002;Evans et al 2005)…”

Section: Current Molecular Gas Amount From Dust Emissionmentioning

confidence: 99%

Search for cold and hot gas in the ram pressure stripped Virgo dwarf galaxy IC 3418

Jáchym¹,

Kenney²,

Růžička³

et al. 2013

A&A

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We present IRAM 30m sensitive upper limits on CO emission in the ram pressure stripped dwarf Virgo galaxy IC3418 and in a few positions covering H ii regions in its prominent 17 kpc UV/Hα gas-stripped tail. In the central few arcseconds of the galaxy, we report a possible marginal detection of about 1 × 10 6 M ⊙ of molecular gas (assuming a Galactic CO-to-H 2 conversion factor) that could correspond to a surviving nuclear gas reservoir. We estimate that there is less molecular gas in the main body of IC3418, by at least a factor of 20, than would be expected from the pre-quenching UV-based star formation rate assuming the typical gas depletion timescale of 2 Gyr. Given the lack of star formation in the main body, we think the H 2 -deficiency is real, although some of it may also arise from a higher CO-to-H 2 factor typical in low-metallicity, low-mass galaxies. The presence of H ii regions in the tail of IC3418 suggests that there must be some dense gas; however, only upper limits of < 1 × 10 6 M ⊙ were found in the three observed points in the outer tail. This yields an upper limit on the molecular gas content of the whole tail < 1 × 10 7 M ⊙ , which is an amount similar to the estimates from the observed star formation rate over the tail. We also present strong upper limits on the X-ray emission of the stripped gas in IC3418 from a new Chandra observation. The measured X-ray luminosity of the IC3418 tail is about 280 times lower than that of ESO 137-001, a spiral galaxy in a more distant cluster with a prominent ram pressure stripped tail. Non-detection of any diffuse X-ray emission in the IC3418 tail may be due to a low gas content in the tail associated with its advanced evolutionary state and/or due to a rather low thermal pressure of the surrounding intra-cluster medium.

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“…It is already known that spiral galaxies contain large amounts of dust (Stickel et al 2000(Stickel et al , 2004Tuffs et al 2002;Popescu et al 2002;Vlahakis et al 2005;Driver et al 2007;Dariush et al 2011;Rowlands et al 2012;Bourne et al 2012;Dale et al 2012;Grootes et al 2013a), and that this dust changes the appearance of disks and bulges from what would be predicted based solely on their intrinsic stellar distributions (e.g. Tuffs et al 2004;Möllenhoff et al 2006;Gadotti et al 2010;Pastrav et al 2013).…”

Section: Introductionmentioning

confidence: 99%

The effects of dust on the photometric parameters of decomposed disks and bulges

Pastrav

Popescu

Tuffs

et al. 2013

A&A

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We present results of a study to quantify the effects of dust on the derived photometric parameters of disk and bulges obtained from bulge-disk decomposition: scale-length, effective radius, Sérsic index, disk axis-ratio, and bulge-to-disk ratio. The dust induced changes in these parameters were obtained by fitting simulated images of composite systems (containing a disk and a bulge) produced using radiative transfer calculations. The simulations were fitted with the GALFIT 3.0.2 data analysis algorithm. Fits were done with both a combination of an exponential plus a variable-index Sérsic function as well as with a combination of two variable-index Sérsic functions. We find that dust is biasing the derived exponential scale-length of decomposed disks towards smaller values than would be otherwise derived if the galaxy were to have no bulge. Similarly, the derived bulge-to-disk ratio is biased towards smaller values. However, the derived axis-ratio of the disk is not changed in the decomposition process. The derived effective radius of decomposed disks of systems having exponential bulges is found to be less affected by dust when fits are done with two variable-index Sérsic functions. For the same type of fits dust is found to bias the value of the derived effective radius of decomposed disks towards lower values for systems having de Vaucouleurs bulges.

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Erratum: “Far‐Infrared Photometry of a Statistical Sample of Late‐Type Virgo Cluster Galaxies” (ApJS, 139, 37 [2002])

Cited by 58 publications

References 0 publications

[C II] emission and star formation in late-type galaxies

[C II] emission and star formation in late-type galaxies

Search for cold and hot gas in the ram pressure stripped Virgo dwarf galaxy IC 3418

The effects of dust on the photometric parameters of decomposed disks and bulges

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