The Three-dimensional Structure of the Virgo Cluster Region from Tully-Fisher and H [CSC]i[/CSC] Data

Solanes, J. M.; Sanchís, T.; Salvador-Solé, E.; Giovanelli, Riccardo; Haynes, Martha P.

doi:10.1086/344074

Cited by 96 publications

(116 citation statements)

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“…The velocity of NGC 4150 is rather low (v = 226 km s −1 ), but it is difficult to say whether it is discordant with either our distance estimate of 14.4 ± 0.7 Mpc or Karachentsev et al's (2003) ≈20 Mpc. Solanes et al (2002) have found that most Virgo galaxies in the region closest to us, corresponding to our distance to NGC 4150, have high radial velocities outward from the cluster centre (with similarly unusually high velocities away from us for Virgo cluster galaxies in the region behind the centre of the cluster). The angular separation of NGC 4150 from the cluster centre is 19 degrees.…”

Section: Discussionmentioning

confidence: 54%

New distances of unresolved dwarf elliptical galaxies in the vicinity of the Local Group

Rekola

Jerjen

Flynn

2005

A&A

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Abstract. We present Surface Brightness Fluctuation distances of nine early-type dwarf galaxies and the S0 galaxy NGC 4150 in the Local Volume based on deep B-and R-band CCD images obtained with the 2.56 m Nordic Optical Telescope. Typically, six stellar fields at various galactocentric distances have been chosen for each galaxy as appropriately free of foreground stars and other contaminants, and Fourier analysed to determine the distances, which are found to lie in the range of 3 to 16 Mpc. The SBF method is thus demonstrated to efficiently measure distances from the ground with mid-aperture telescopes for galaxies for which only the tip of the red giant branch method in combination with the Hubble Space Telescope has been available until now. We obtained the following distance moduli: 28.11 ± 0.15 mag (or 4.2 ± 0.3 Mpc) for UGC 1703, 27.61 ± 0.17 mag (or 3.3 ± 0.3 Mpc) for KDG 61, 29.00 ± 0.27 mag (or 6.3 ± 0.8 Mpc) for UGCA 200, 27.74 ± 0.18 mag (or 3.5 ± 0.3 Mpc) for UGC 5442, 30.22 ± 0.17 mag (or 11.1 ± 0.9 Mpc) for UGC 5944, 30.79 ± 0.11 mag (or 14.4 ± 0.7 Mpc) for NGC 4150, 31.02 ± 0.25 mag (or 16.0 ± 1.9 Mpc) for BTS 128, 29.27 ± 0.16 mag (or 7.1 ± 0.6 Mpc) for UGC 7639, 30.19 ± 0.23 mag (or 10.9 ± 1.2 Mpc) for UGC 8799 with an alternative distance of 30.61 ± 0.26 mag (or 13.2 ± 1.7 Mpc), and 29.60 ± 0.20 mag (or 8.3 ± 0.8 Mpc) for UGC 8882.

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Section: Discussionmentioning

confidence: 54%

New distances of unresolved dwarf elliptical galaxies in the vicinity of the Local Group

Rekola

Jerjen

Flynn

2005

A&A

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“…more than twice the distance of the Milky Way from the center of the cluster (∼17 Mpc). Solanes et al (2002), starting from the HI distribution, reconstructed the structure of the cluster, and found galaxies with elongated gas-tails, due to environmental effects, out to cluster centre distances of 25-30 Mpc. These results imply that at the distance of NGC 4189 from the cluster center it is still possible to find galaxies that are Virgo members.…”

Section: Appendix A: Notes On Individual Objectsmentioning

confidence: 99%

TheHerschelVirgo Cluster Survey

Pappalardo

Bianchi

Corbelli

et al. 2012

A&A

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Aims. We investigate the dust-to-gas mass ratio and the environmental effects on the various components of the interstellar medium for a spatially resolved sample of Virgo spirals. Methods. We have used the IRAM-30 m telescope to map over their full extent NGC 4189, NGC 4298, NGC 4388, and NGC 4299 in the 12 CO(1-0) and the 12 CO(2-1) lines. We observed the same lines in selected regions of NGC 4351, NGC 4294, and NGC 4424. The CO observations are combined with Herschel maps in 5 bands between 100-500 μm from the HeViCS survey, and with HI data from the VIVA survey, to obtain spatially resolved dust and gas distributions. We studied the environmental dependencies by adding to our sample eight galaxies with 12 CO(1-0) maps from the literature. Results. We estimate the integrated mass of molecular hydrogen for the galaxies observed in the CO lines. We find molecular-to-total gas mass fractions between 0.04 ≤ f mol ≤ 0.65, with the lowest values for the dimmest galaxy in the B-band. The integrated dust-togas ratio ranges between 0.011 and 0.004. For the 12 mapped galaxies we derive the radial distributions of the atomic gas, molecular gas, and dust. We also study the effect of different CO-to-H 2 conversion factors. Both the molecular gas and the dust distributions show steeper radial profiles for HI-deficient galaxies and the average dust-to-gas ratio for these galaxies increases or stays radially constant. On scales of ∼3 kpc, we find a strong correlation between the molecular gas and the 250 μm surface brightness that is tighter than average for non-deficient galaxies. The correlation becomes linear if we consider the total gas surface mass density. However, the inclusion of atomic hydrogen does not improve the statistical significance of the correlation. Conclusions. The environment can modify the distributions of molecules and dust within a galaxy, although these components are more tightly bound than the atomic gas.

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“…Calculation of the H I masses of these clouds is somewhat hampered by the uncertain distance of the objects. These clouds are in within the regions of the W and W structures identified by de Vaucouleurs (1961), which are farther away than the Virgo cluster proper (e.g., Solanes et al 2002). We note that the gas-rich spiral galaxy VCC297 is close to the PG1216 + 069 sight line, and the H I emission of VCC297 indicates a redshift that is quite close to the redshift of the sub-DLA and the other starless H I clouds in this field (see Figure 2).…”

Section: Starless H I Clouds In the X-ray Bright Ngc4261 Galaxy Groupmentioning

confidence: 93%

“…We note that the gas-rich spiral galaxy VCC297 is close to the PG1216 + 069 sight line, and the H I emission of VCC297 indicates a redshift that is quite close to the redshift of the sub-DLA and the other starless H I clouds in this field (see Figure 2). Thus, it is reasonable to suppose that the H I clouds are at the same distance as VCC297; the Tully-Fisher method indicates a distance of 23.4 Mpc for VCC297 (Solanes et al 2002). On the other hand, the clouds are close to the NGC4261 loose group, and they could be at the distance of the galaxy group.…”

Section: Starless H I Clouds In the X-ray Bright Ngc4261 Galaxy Groupmentioning

confidence: 98%

Connecting Lost Baryons and Dark Galaxies via QSO Absorption Lines

Tripp

2007

Proc. IAU

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Abstract. QSO absorption lines are sensitive to very low density gas, and consequently, QSO spectroscopy provides a powerful tool for measuring the distribution, physical conditions, and metal enrichment of baryons in the intergalactic medium and in "dark galaxies". However, ultraviolet spectroscopy is required to study QSO absorbers in the nearby universe where the connections between the absorbing gas and galaxies/environment can be probed. This talk reviewed several recent studies of low−z QSO absorbers in order to demonstrate the value of combining high-resolution ultraviolet spectroscopy with complementary information on the absorber environment, e.g., mapping of 21 cm emission in the vicinity of the absorbers; some notes on these examples are presented in this paper. The absorbers probed range from high−N (H I) damped Lyman α absorbers down to very low-column Lyα forest clouds with log N (H I) < 13.5. The high−N (H I) systems are candidate "dark galaxies" -these systems are more metal enriched than the high−z IGM, possibly due to in-situ star formation, and some of the absorbers are highly metal enriched. However, we have obtained follow-up 21cm emission mapping with the VLA and deep optical imaging, and while we do find H I clouds associated with the absorbers in 21cm emission, we often do not find any evidence of in-situ stars. At this juncture, it seems more likely that these low−z absorbers were enriched with metals within galaxies and were subsequently transported out into the IGM, e.g., by tidal stripping or galactic winds. This contribution also summarizes some recent results on the search for lost baryons in the "warm-hot" (shock-heated) low-redshift IGM.

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The Three-dimensional Structure of the Virgo Cluster Region from Tully-Fisher and H [CSC]i[/CSC] Data

Cited by 96 publications

References 44 publications

New distances of unresolved dwarf elliptical galaxies in the vicinity of the Local Group

New distances of unresolved dwarf elliptical galaxies in the vicinity of the Local Group

TheHerschelVirgo Cluster Survey

Connecting Lost Baryons and Dark Galaxies via QSO Absorption Lines

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