2003
DOI: 10.1086/345537
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The Cool Interstellar Medium in S0 Galaxies. I. A Survey of Molecular Gas

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Cited by 119 publications
(147 citation statements)
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“…The total gas mass of NGC 4438 calculated as the sum of the molecular gas mass derived from our observations and the initial H mass of NGC 4501 gives 3.4 × 10 9 M . The total gas mass for NGC 4435 represents the upper limit for an S0 galaxy of its luminosity (Welch & Sage 2003). The ensemble of model clouds has a power law mass distribution as described in Vollmer et al (2001).…”
Section: Simulationsmentioning
confidence: 99%
“…The total gas mass of NGC 4438 calculated as the sum of the molecular gas mass derived from our observations and the initial H mass of NGC 4501 gives 3.4 × 10 9 M . The total gas mass for NGC 4435 represents the upper limit for an S0 galaxy of its luminosity (Welch & Sage 2003). The ensemble of model clouds has a power law mass distribution as described in Vollmer et al (2001).…”
Section: Simulationsmentioning
confidence: 99%
“…Also, perhaps the slope of the ionized gas velocity profile in our data may be slightly underestimated due to moderate seeing quality of the observations of March 2002. The maximum gas rotation velocity, ∼ 250 km/s at R = 5 ′′ −10 ′′ which may be transformed into 450 km/s under i = 34 • , seems to be enormous; but this result is confirmed by recent CO observations of NGC 3607 according to which 2.3 · 10 8 M⊙ of the molecular gas within R = 5 ′′ rotates at a speed of 250 km/s (Welch & Sage 2002). Interestingly, in the integrated molecular-line profile only a receding horn is well seen -the asymmetry is quite similar to that of the Fig.…”
Section: Ngc 3607mentioning
confidence: 76%
“…The result of the test is that the M H 2 distribution of CoreG and PlawG are not drawn from different parent populations with a confidence level greater than 95%. Welch & Sage (2003), OC10 Ocaña Flaquer et al (2010), WI95 Wiklind et al (1995), HU94 Huchtmeier et al (1994), SO93 Sofue & Wakamatsu (1993), SA07 Sage et al (2007), SA89 Sage & Wrobel (1989), TA94 Taniguchi et al (1994), MA97 Maiolino et al (1997), VO05 Vollmer et al (2005); nuclear luminosities [erg s −1 ] from and in (5) radio, (6) optical, and (7) and X-ray (2-10 keV); In Fig. 4 we compare the molecular masses and stellar luminosity, L * , estimated from the K-band absolute magnitude of the galaxy.…”
Section: H 2 Mass For the Sample Of Nearby Etgsmentioning
confidence: 99%