Discovery of a Very Extended Emission‐Line Region around the Seyfert 2 Galaxy NGC 4388

Yoshida, Michitoshi; Yagi, Masafumi; Okamura, S.; Aoki, Kentaro; Ohyama, Youichi; Komiyama, Yutaka; Yasuda, Naoki; Iye, Masanori; Kashikawa, Nobunari; Doi, Mamoru; Furusawa, Hisanori; Hamabe, M.; Kimura, Masahiko; Miyazaki, Masayuki; Miyazaki, Satoshi; Nakata, Fumiaki; Ouchi, Masami; Sekiguchi, M.; Shimasaku, Kazuhiro; Oda, Hiroshi

doi:10.1086/338353

Cited by 100 publications

(137 citation statements)

References 49 publications

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“…The newly formed stars are mainly concentrated in the compressed residual disc. Like in the observations of Yoshida et al (2002Yoshida et al ( , 2004 some Hα emitting gas can be found several kpc behind the ram pressure affected disc in the forming gaseous wake.…”

Section: The Distribution Of the Different Componentssupporting

confidence: 70%

“…They conclude that the most plausible formation mechanism for these star forming regions is ram-pressure stripping. Another example how ram pressure stripping influences the gaseous disc and the stripped material is presented in Yoshida et al (2004Yoshida et al ( , 2002. They investigated NGC 4388, a Seyfert 2 Virgo cluster galaxy, with deep optical spectroscopy.…”

Section: Comparison With Observationsmentioning

confidence: 99%

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The effect of ram pressure on the star formation, mass distribution and morphology of galaxies

Kapferer¹,

Sluka²,

Schindler³

et al. 2009

A&A

208

253

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Aims. We investigate the dependence of star formation and the distribution of the components of galaxies on the strength of ram pressure. Several mock observations in X-ray, Hα and HI wavelength for different ram-pressure scenarios are presented. Methods. By applying a combined N-body/hydrodynamic description (GADGET-2) with radiative cooling and a recipe for star formation and stellar feedback 12 different ram-pressure stripping scenarios for disc galaxies were calculated. Special emphasis was put on the gas within the disc and in the surroundings. All gas particles within the computational domain having the same mass resolution. The relative velocity was varied from 100 km s −1 to 1000 km s −1 in different surrounding gas densities in the range from 1 × 10 −28 to 5 × 10 −27 g/cm 3 . The temperature of the surrounding gas was initially 1 × 10 7 K. Results. The star formation of a galaxy is enhanced by more than a magnitude in the simulation with a high ram-pressure (5 × 10 −11 dyn/cm 2 ) in comparison to the same system evolving in isolation. The enhancement of the star formation depends more on the surrounding gas density than on the relative velocity. Up to 95% of all newly formed stars can be found in the wake of the galaxy out to distances of more than 350 kpc behind the stellar disc. Continuously stars fall back to the old stellar disc, building up a bulge-like structure. Young stars can be found throughout the stripped wake with surface densities locally comparable to values in the inner stellar disc. Ram-pressure stripping can shift the location of star formation from the disc into the wake on very short timescales. As the gas in a galaxy has a complex velocity pattern due to the rotation and spiral arms, the superposition of the internal velocity field and the ram pressure causes complex structures in the gaseous wake which survive dynamically up to several 100 Myr. Finally we provide simulated X-ray, Hα and HI observations to be able to compare our results with observations in these wavebands. These simulated observations show many features which depend strongly both on the strength and the duration of the external ram pressure.

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Section: The Distribution Of the Different Componentssupporting

confidence: 70%

Section: Comparison With Observationsmentioning

confidence: 99%

The effect of ram pressure on the star formation, mass distribution and morphology of galaxies

Kapferer¹,

Sluka²,

Schindler³

et al. 2009

A&A

208

253

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“…The galaxy is one of the most HI-deficient in our sample (def HI = 1.16), showing HI distribution truncated within the optical disk (Chung et al 2009a). Yoshida et al (2002) found that the Hα emission extends for 35 kpc in the north east direction. Vollmer & Huchtmeier (2003) found HI gas out to 20 kpc along the same direction as the Hα emission.…”

Section: Appendix A: Notes On Individual Objectsmentioning

confidence: 60%

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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“…By observing the galaxy in Hα Veilleux et al (1999b) found a large plume of ionized gas extending 4 kpc above the plane. In subsequent SUBARU observations Yoshida et al (2002) reveal a more extended tail out to 35 kpc to the northeast. Vollmer & Huchtmeier (2003) performed 21-cm line observations with the Effelsberg 100-m radio telescope.…”

Section: Introductionmentioning

confidence: 86%

Pinning down the ram-pressure-induced halt of star formation in the Virgo cluster spiral galaxy NGC 4388

Pappalardo¹,

Lançon²,

Vollmer³

et al. 2010

A&A

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Context. In a galaxy cluster, the evolution of spiral galaxies depends on their cluster environment. Ram pressure due to the rapid motion of a spiral galaxy within the hot intracluster medium removes the galaxy's interstellar medium from the outer disk. Once the gas has left the disk, star formation stops. The passive evolution of the stellar populations should be detectable in optical spectroscopy and multi-wavelength photometry. Aims. The goal of our study is to recover the stripping age of the Virgo spiral galaxy NGC 4388, i.e. the time elapsed since the halt of star formation in the outer galactic disk using a combined analysis of optical spectra and photometry. Methods. We performed VLT FORS2 long-slit spectroscopy of the inner star-forming and outer gas-free disk of NGC 4388. We developed a non-parametric inversion tool that allows us to reconstruct the star formation history of a galaxy from spectroscopy and photometry. The tool was tested on a series of mock data using Monte Carlo simulations. The results from the non-parametric inversion were refined by applying a parametric inversion method. Results. The star formation history of the unperturbed galactic disk is flat. The non-parametric method yields a rapid decline of star formation < ∼ 200 Myr ago in the outer disk. The parametric method is not able to distinguish between an instantaneous and a longlasting star formation truncation. We find that 190 ± 30 Myr ago the star formation reached half of its pre-stripping value. Conclusions. We are able to give a precise stripping age that is consistent with revised dynamical models.

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Discovery of a Very Extended Emission‐Line Region around the Seyfert 2 Galaxy NGC 4388

Cited by 100 publications

References 49 publications

The effect of ram pressure on the star formation, mass distribution and morphology of galaxies

The effect of ram pressure on the star formation, mass distribution and morphology of galaxies

TheHerschelVirgo Cluster Survey

Pinning down the ram-pressure-induced halt of star formation in the Virgo cluster spiral galaxy NGC 4388

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