Testing the gravitational field in elliptical galaxies - NGC 5077

Bertola, F.; Bettoni, D.; Danziger, John; Sadler, E. M.; Sparke, L. S.; Dezeeuw, T

doi:10.1086/170058

Cited by 156 publications

(147 citation statements)

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“…In order to obtain the value of the systemic velocity and the rotation velocity field of the disk of the galaxy, we modeled the stellar velocity field assuming a spherical potential with pure circular motions, with the observed radial velocity at a position (R, ψ) in the plane of the sky given by (Bertola et al 1991):…”

Section: The Stellar Kinematicsmentioning

confidence: 99%

Gas inflows towards the nucleus of the Seyfert 2 galaxy NGC 1667

Schnorr-Müller

Storchi‐Bergmann

Ferrari

et al. 2017

Mon. Not. R. Astron. Soc.

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We use optical spectra from the inner 2 × 3 kpc 2 of the Seyfert 2 galaxy NGC 1667, obtained with the GMOS integral field spectrograph on the Gemini South telescope at a spatial resolution of ≈ 240 pc, to assess the feeding and feedback processes in this nearby AGN. We have identified two gaseous kinematical components in the emission line profiles: a broader component (σ ≈ 400 km s −1 ) which is observed in the inner 1-2 ′′ and a narrower component (σ ≈ 200 km s −1 ) which is present over the entire field-ofview. We identify the broader component as due to an unresolved nuclear outflow. The narrower component velocity field shows strong isovelocity twists relative to a rotation pattern, implying the presence of strong non-circular motions. The subtraction of a rotational model reveals that these twists are caused by outflowing gas in the inner ≈ 1 ′′ , and by inflows associated with two spiral arms at larger radii. We calculate an ionized gas mass outflow rate ofṀ out ≈ 0.16 M ⊙ yr −1 . We calculate the net gas mass flow rate across a series of concentric rings, obtaining a maximum mass inflow rate in ionized gas of ≈ 2.8 M ⊙ year −1 at 800 pc from the nucleus, which is two orders of magnitude larger than the accretion rate necessary to power this AGN. However, as the mass inflow rate decreases at smaller radii, most of the gas probably will not reach the AGN, but accumulate in the inner few hundred parsecs. This will create a reservoir of gas that can trigger the formation of new stars.

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Section: The Stellar Kinematicsmentioning

confidence: 99%

Gas inflows towards the nucleus of the Seyfert 2 galaxy NGC 1667

Schnorr-Müller

Storchi‐Bergmann

Ferrari

et al. 2017

Mon. Not. R. Astron. Soc.

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“…The parameters derived from the fit are: systemic velocity corrected to the heliocentric reference frame V s = 2332 ± 15 km s −1 , Ψ 0 = 162 • ± 0.6 • , A = 306 ± 10.5 km s −1 , i = 43 • ± 2.5 • , c 0 = 0.9 ± 0.04 arcsec. The location of the kinematical center was fixed at X 0 = Y 0 = 0 arcsec and p was limited to range between 1 and 1.5, which is the range of values expected for galaxies (Bertola et al 1991). The best fit was obtained with p = 1.5.…”

Section: Channel Mapsmentioning

confidence: 99%

Feeding versus feedback in AGN from near-infrared IFU observations XI: NGC 2110

Diniz

Riffel

Storchi‐Bergmann

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a two-dimensional mapping of the gas flux distributions, as well as of the gas and stellar kinematics in the inner 220 pc of the Seyfert galaxy NGC 2110, using K-band integral field spectroscopy obtained with the Gemini NIFS at a spatial resolution of ≈ 24 pc and spectral resolution of ≈ 40 km s −1 . The H 2 λ 2.1218 µm emission extends over the whole field-of-view and is attributed to heating by X-rays from the AGN and/or by shocks, while the Brγ emission is restricted to a bi-polar region extending along the South-East-NorthWest direction. The masses of the warm molecular gas and of the ionized gas are M H 2 ≈ 1.4 × 10 3 M ⊙ and M H II ≈ 1.8 × 10 6 M ⊙ , respectively. The stellar kinematics present velocity dispersions reaching 250 km s −1 , and a rotation pattern reaching an amplitude of 200 km s −1 . The gas velocity fields present a similar rotation pattern but also additional components that we attribute to inflows and outflows most clearly observed in the molecular gas emission. The inflows are observed beyond the inner 70 pc and are associated to a spiral arm seen in blueshift to the North-East and another in redshift to the South-West. We have estimated a mass inflow rate in warm molecular gas of ≈ 4.6 × 10 −4 M ⊙ yr −1 . Within the inner 70 pc, another kinematic component is observed in the H 2 emission that can be interpreted as due to a bipolar nuclear outflow oriented along the East-West direction, with a mass-outflow rate of ≈ 4.3 × 10 −4 M ⊙ yr −1 in warm H 2 .

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“…According to Bertola et al (1991), this assumption results in an observed radial circular velocity v(r,ψ) in the plane of the sky given by (see Eq. (2) in their paper):…”

Section: Gas and Stellar Kinematicsmentioning

confidence: 99%

Broad-band photometry and long-slit spectroscopy of the peculiar ring galaxy FM 287-14

Faúndez-Abans

Rocha-Poppe

Fernandes-Martin

et al. 2013

A&A

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Aims. We report detailed morphological and kinematical insights into the disturbed galaxy FM 287-14, which is reported in the literature as a member of strongly interacting galaxies with a clear case of mergers. The main purpose of this paper is to provide a first observational study of this double-nuclei object based on photometry and spectroscopy. Methods. The study is based on BVR photometry with the 1.6-m telescope at OPD, and long-slit spectroscopy with Gemini South's GMOS spectrograph, with two-gratings centered at 5 011 Å and 6 765 Å. Image enhancement techniques were applied to the direct images, and the main lines in the spectra were used to determine the radial velocity. Line ratios and color-color diagnostic diagrams helped determine the nature of this object.Results. The external NE section is populated with well-defined H ii regions and is bluer than the SW region with less evidence of H ii regions. A double nucleus has been identified. The (B − R) × (B − V) diagram shows that the main nucleus is redder than the second one; the internal "ring-like" structure is redder than the external one. The main object redshift is z = 0.0311, corresponding to a line-of-sight velocity of 9334 km s −1 (a distance of 133.3 Mpc), and the second nucleus has a redshift of z = 0.0310, corresponding to a line-of-sight velocity of 9300 km s −1 (a distance of 132.9 Mpc). Both nuclei show characteristics of early-type galaxies, but the main one also shows modest emission evidence of the [N ii]λ6583 line.Conclusions. The peculiarities of FM 287-14 can be adequately interpreted as an ongoing merging-stage of interaction of the main object with a companion galaxy.

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Testing the gravitational field in elliptical galaxies - NGC 5077

Cited by 156 publications

References 0 publications

Gas inflows towards the nucleus of the Seyfert 2 galaxy NGC 1667

Gas inflows towards the nucleus of the Seyfert 2 galaxy NGC 1667

Feeding versus feedback in AGN from near-infrared IFU observations XI: NGC 2110

Broad-band photometry and long-slit spectroscopy of the peculiar ring galaxy FM 287-14

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