Volume 556, August 2013
|Number of page(s)||15|
|Published online||02 August 2013|
Astronomical Institute, Academy of Sciences of the Czech
Boční II 1401,
2 Department of Astronomy, Yale University, 260 Whitney Ave., New Haven, CT 06511, USA
3 Eureka Scientific, 2452 Delmer Street Suite 100, Oakland, CA 94602, USA
4 Observatoire de Paris, LERMA, 61 Av. de l’Observatoire, 75014 Paris, France
Accepted: 30 April 2013
We present IRAM 30 m sensitive upper limits on CO emission in the ram pressure stripped dwarf Virgo galaxy IC 3418 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 × 106 M⊙ of molecular gas (assuming a Galactic CO-to-H2 conversion factor) that could correspond to a surviving nuclear gas reservoir. We estimate that there is less molecular gas in the main body of IC 3418, 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 H2-deficiency is real, although some of it may also arise from a higher CO-to-H2 factor typical in low-metallicity, low-mass galaxies. The presence of H ii regions in the tail of IC 3418 suggests that there must be some dense gas; however, only upper limits of <1 × 106 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 × 107 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 IC 3418 from a new Chandra observation. The measured X-ray luminosity of the IC 3418 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 IC 3418 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.
Key words: galaxies: individual: VCC 1217/IC 3418 / galaxies: clusters: individual: Virgo / galaxies: evolution / galaxies: ISM / ISM: kinematics and dynamics / methods: observational
Based on observations carried out with the IRAM 30 m Telescope and with the Chandra X-ray Observatory. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).
CO spectra as FITS files are available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/556/A99
© ESO, 2013
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