The distribution of ionized gas in early-type
galaxies. 
II. The velocity field of the ionized gas

Zeilinger, W. W.; Pizzella, A.; Amico, Paola; Bertin, G.; Bertola, F.; Buson, L. M.; Danziger, I. J.; Dejonghe, Herwig; Sadler, E. M.; Saglia, R.; Zeeuw, P. T. de

doi:10.1051/aas:1996290

Cited by 32 publications

(30 citation statements)

References 17 publications

(22 reference statements)

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…This is indeed confirmed by observations, showing regular gaseous disk structures and coherent gas motions (see e.g. Zeilinger et al 1996;Sarzi et al 2006). If most of the clouds were to rotate in the same direction, it would then be rather difficult for them to collide at the high speed required.…”

Section: Comparison With Modelssupporting

confidence: 76%

“…This scenario cannot be excluded since several studies have found a gaseous component of high velocity dispersion, in the range 150-250 km s −1 , in the center of early-type galaxies (e.g. Bertola et al 1995;Zeilinger et al 1996;Sarzi et al 2006), which translates into higher intrinsic 3D velocity dispersions. This scenario is very appealing since it would naturally explain the observed trends between the emission strength, and the [NII]/Hα ratio, with the galaxy stellar central velocity dispersion.…”

Section: The Ionization Mechanism In Linersmentioning

confidence: 99%

“…If most of the clouds were to rotate in the same direction, it would then be rather difficult for them to collide at the high speed required. On the other hand, observations detect an additional gaseous component of high gas velocity dispersion, in the range 150-250 km s −1 (Bertola et al 1995;Zeilinger et al 1996;Emsellem et al 2003). Sarzi et al (2006) found that σ gas is generally smaller than the stellar velocity dispersion σ * , but in some cases σ gas ∼ σ * , either only in the central regions or over most of the field.…”

Section: Comparison With Modelsmentioning

confidence: 99%

“…The first problem is the origin of the ISM in ETGs. Narrowband imaging centered around Hα+ [NII]λ6584 shows that the ionized gas has a variety of morphologies, from regular, disklike structures, to filamentary structures (Demoulin-Ulrich et al 1984;Buson et al 1993;Macchetto et al 1996;Zeilinger et al 1996;Martel et al 2004;Sarzi et al 2006). Evidence of the acquisition of external gas comes from kinematical studies showing that the angular momentum of the gas is often decoupled from that of the stars (Bertola et al 1992;van Dokkum & Franx 1995;Caon et al 2000), even if according to Sarzi et al (2006) the angular momenta are inconsistent with a purely external origin for the gas.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Nearby early-type galaxies with ionized gas

Annibali

Bressan

Rampazzo

et al. 2010

A&A

Self Cite

121

162

View full text Add to dashboard Cite

Aims. A significant fraction of early-type galaxies (ETGs) exhibit emission lines in their optical spectra. We attempt to identify the producing the emission mechanism and the ionized gas in ETGs, and its connection with the host galaxy evolution. Methods. We analyzed intermediate-resolution optical spectra of 65 ETGs, mostly located in low density environments and exhibiting spectros-copic diagnostic lines of ISM from which we had previously derived stellar population properties. To extract the emission lines from the galaxy spectra, we developed a new fitting procedure that accurately subtracts the underlying stellar continuum, and accounts for the uncertainties caused by the age-metallicity degeneracy. Results. Optical emission lines are detected in 89% of the sample. The incidence and strength of emission correlate with neither the E/S0 classification, nor the fast/slow rotator classification. By means of the classical [OIII]/Hβ versus [NII]/Hα diagnostic diagram, the nuclear galaxy activity is classified such that 72% of the galaxies with emission are LINERs, 9% are Seyferts, 12% are composite/transition objects, and 7% are non-classified. Seyferts have young luminostiy-weighted ages ( 5 Gyr), and appear, on average, significantly younger than LINERs and composites. Excluding the Seyferts from our sample, we find that the spread in the ([OIII], Hα, or [NII]) emission strength increases with the galaxy central velocity dispersion σ c . Furthermore, the [NII]/Hα ratio tends to increase with σ c . The [NII]/Hα ratio decreases with increasing galactocentric distance, indicative of either a decrease in the nebular metallicity, or a progressive "softening" of the ionizing spectrum. The average nebular oxygen abundance is slightly less than solar, and a comparison with the results obtained in Paper III from Lick indices shows that it is ≈0.2 dex lower than that of stars. Conclusions. The nuclear (r < r e /16) emission can be attributed to photoionization by PAGB stars alone only for ≈22% of the LINER/composite sample. On the other hand, we cannot exclude an important role of PAGB star photoionization at larger radii. For the major fraction of the sample, the nuclear emission is consistent with excitation caused by either a low-accretion rate AGN or fast shocks (200-500 km s −1 ) in a relatively gas poor environment (n 100 cm −3 ), or both. The derived [SII]6717/6731 ratios are consistent with the low gas densities required by the shock models. The derived nebular metallicities are indicative of either an external origin of the gas, or an overestimate of the oxygen yields by SN models.

show abstract

Section: Comparison With Modelssupporting

confidence: 76%

Section: The Ionization Mechanism In Linersmentioning

confidence: 99%

Section: Comparison With Modelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Nearby early-type galaxies with ionized gas

Annibali

Bressan

Rampazzo

et al. 2010

A&A

Self Cite

121

162

View full text Add to dashboard Cite

show abstract

“…Buson et al (1993) and Zeilinger et al (1996) also found that the warm ionized gas is misaligned relative to the stars in NGC 1453, though with a larger misalignment angle of ≈128°.I ti s unlikely that stellar mass loss from the old stellar population is the primary source of the warm ionized medium in NGC 1453 because such recycled gas would tend to remain in the potential well of the stars, leading to photometric and kinematic alignment between the stars and gas.…”

Section: External Accretion Versus Internal Originsmentioning

confidence: 96%

The MASSIVE Survey. VI. The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Early-type Galaxies

Pandya

Greene

et al. 2017

ApJ

View full text Add to dashboard Cite

Vous avez des questions? Nous pouvons vous aider. Pour communiquer directement avec un auteur, consultez la première page de la revue dans laquelle son article a été publié afin de trouver ses coordonnées. Si vous n'arrivez pas à les repérer, communiquez avec nous à PublicationsArchive-ArchivesPublications@nrc-cnrc.gc.ca. Questions? Contact the NRC Publications Archive team atPublicationsArchive-ArchivesPublications@nrc-cnrc.gc.ca. If you wish to email the authors directly, please see the first page of the publication for their contact information. NRC Publications Archive Archives des publications du CNRCThis publication could be one of several versions: author's original, accepted manuscript or the publisher's version. / La version de cette publication peut être l'une des suivantes : la version prépublication de l'auteur, la version acceptée du manuscrit ou la version de l'éditeur. For the publisher's version, please access the DOI link below./ Pour consulter la version de l'éditeur, utilisez le lien DOI ci-dessous.http://doi.org/10.3847/1538-4357/aa5ebcAccess and use of this website and the material on it are subject to the Terms and Conditions set forth atThe massive survey VI: the spatial distribution and kinematics of warm ionized gas in the most massive local early-type galaxies Pandya, Viraj; Greene, Jenny E.; Ma, Chung-Pei; Veale, Melanie; Ene, Irina; Davis, Timothy A.; Blakeslee, John P.; Goulding, Andy D.; McConnell, Nicholas J.; Nyland, Kristina; Thomas, Jens http://nparc.cisti-icist.nrc-cnrc.gc.ca/fra/droits L'accès à ce site Web et l'utilisation de son contenu sont assujettis aux conditions présentées dans le site LISEZ CES CONDITIONS ATTENTIVEMENT AVANT D'UTILISER CE SITE WEB. NRC Publications Record / Notice d'Archives des publications de CNRC:http://nparc.cisti-icist.nrc-cnrc.gc.ca/eng/view/object/?id=f69bb12a-dd71-4a0f-a3e2-67cd7d1de13a http://nparc.cisti-icist.nrc-cnrc.gc.ca/fra/voir/objet/?id=f69bb12a-dd71-4a0f-a3e2-67cd7d1de13a AbstractWe present the first systematic investigation of the existence, spatial distribution, and kinematics of warm ionized gas as traced by the [O II] 3727 Å emission line in 74 of the most massive galaxies in the local universe. All of our galaxies have deep integral-field spectroscopy from the volume-and magnitude-limited MASSIVE survey of earlytype galaxies with stellar mass ()  * > MM log 11.5 (M K <−25.3 mag) and distance D<108 Mpc. Of the 74 galaxies in our sample, we detect warm ionized gas in 28, which yields a global detection fraction of 38±6% down to a typical [O II] equivalent width limit of 2 Å. MASSIVE fast rotators are more likely to have gas than MASSIVE slow rotators with detection fractions of 80±10% and 28±6%, respectively. The spatial extents span a wide range of radii (0.6-18.2 kpc; 0.1-4R e ), and the gas morphologies are diverse, with 17/28≈61±9% being centrally concentrated, 8/28≈29±9% exhibiting clear rotation out to several kiloparsecs, and 3/28≈11±6% being extended but patchy. Three out of four fast rotators show ki...

show abstract

Origin and Ionization of the Warm Ionized Gas in Massive Early-type Galaxies

Yan¹,

Blanton²

2012

Proc. IAU

View full text Add to dashboard Cite

Abstract. Most early-type galaxies are not devoid of cold and warm gas. The origin and ionization of this gas reveal the intriguing ongoing evolution of these galaxies. In most cases, the warm ionized gas shows emission-line spectra similar to low-ionization nuclear emission-line regions (LINERs). Their ionization mechanism has been hotly debated. We will present evidence from line ratio gradient that rules out AGN and shocks as the dominant ionization mechanism, and suggests the ionizing sources follow the stellar density profile. Hot evolved stars are the favorite candidates but bring new puzzles.This finding allows us to obtain a gas-phase metallicity calibration in these early-type galaxies, using the line emission. We will show how the metallicity of the warm gas depends on stellar mass and stellar age, and what it tells us about the origin of the warm gas in these galaxies.

show abstract

The distribution of ionized gas in early-type galaxies. II. The velocity field of the ionized gas

Cited by 32 publications

References 17 publications

Nearby early-type galaxies with ionized gas

Nearby early-type galaxies with ionized gas

The MASSIVE Survey. VI. The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Early-type Galaxies

Origin and Ionization of the Warm Ionized Gas in Massive Early-type Galaxies

Contact Info

Product

Resources

About