A Digital Archive of H
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                    21 Centimeter Line Spectra of Optically Targeted Galaxies

Springob, Christopher M.; Haynes, Martha P.; Giovanelli, Riccardo; Kent, Brian R.

doi:10.1086/431550

Cited by 472 publications

(615 citation statements)

References 48 publications

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“…The systemic velocity corrected to the heliocentric reference frame is 4570 ±15 km s −1 (taking into account both errors in the measurement and the fit). This value is in good agreement with previous determinations based on optical and H I 21 cm measurements (Springob et al 2005;Radovich & Rafanelli 1996). The model velocity field is shown in Fig.…”

Section: The Stellar Kinematicssupporting

confidence: 93%

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 Kinematicssupporting

confidence: 93%

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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“…Single-dish observations gave intermediate values, consistent with our value within about 1σ: S tot = 2.96 ± 0.51 Jy km s −1 (Matthews et al 2001) and S tot = 3.07 ± 0.36 Jy km s −1 (Springob et al 2005) (this latter value is without the correction for H I self absorption). H I masses were estimated using the luminosity distance D L , given by:…”

Section: H I Data Analysissupporting

confidence: 90%

Structure and dynamics of giant low surface brightness galaxies

Lelli

Fraternali

Sancisi

2010

A&A

141

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Giant low surface brightness (GLSB) galaxies are commonly thought to be massive, dark matter dominated systems. However, this conclusion is based on highly uncertain rotation curves. We present here a new study of two prototypical GLSB galaxies: Malin 1 and NGC 7589. We re-analysed existing H I observations and derived new rotation curves, which were used to investigate the distributions of luminous and dark matter in these galaxies. In contrast to previous findings, the rotation curves of both galaxies show a steep rise in the central parts, typical of high surface brightness (HSB) systems. Mass decompositions with a dark matter halo show that baryons may dominate the dynamics of the inner regions. Indeed, a "maximum disk" fit gives stellar mass-to-light ratios in the range of values typically found for HSB galaxies. These results, together with other recent studies, suggest that GLSB galaxies are systems with a double structure: an inner HSB early-type spiral galaxy and an outer extended LSB disk. We also tested the predictions of MOND: the rotation curve of NGC 7589 is reproduced well, whereas Malin 1 represents a challenging test for the theory.

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“…Huchtmeier & Richter (1989) report a singledish flux of 8.83 Jy km s −1 , while Springob et al (2005) give a corrected 2 single-dish flux of 13.9 Jy km s −1 . Although these flux measurements are of the same order, they show a relatively large spread, which is caused by a combination of different effects.…”

Section: The Datamentioning

confidence: 99%

“…Huchtmeier & Richter (1989) report a single-dish flux of 17.9 Jy km s −1 , which was corrected to 18.9 Jy km s −1 by Springob et al (2005).…”

Section: The Datamentioning

confidence: 99%

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HERschelObservations of Edge-on Spirals (HEROES)

Allaert

Gentile

Baes

et al. 2015

A&A

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Context. Edge-on galaxies can offer important insight into galaxy evolution because they are the only systems where the distribution of the different components can be studied both radially and vertically. The HEROES project was designed to investigate the interplay between the gas, dust, stars, and dark matter (DM) in a sample of 7 massive edge-on spiral galaxies. Aims. In this second HEROES paper, we present an analysis of the atomic gas content of 6 out of 7 galaxies in our sample. The remaining galaxy was recently analysed according to the same strategy. The primary aim of this work is to constrain the surface density distribution, the rotation curve, and the geometry of the gas disks in a homogeneous way. In addition we identify peculiar features and signs of recent interactions. Methods. We have constructed detailed tilted-ring models of the atomic gas disks based on new GMRT 21-cm observations of NGC 973 and UGC 4277 and re-reduced archival H  data of NGC 5907, NGC 5529, IC 2531, and NGC 4217. Potential degeneracies between different models were resolved by requiring good agreement with the data in various representations of the data cubes. Results. From our modelling we find that all but one galaxy are warped along the major axis. In addition, we identify warps along the line of sight in three galaxies. A flaring gas layer is required to reproduce the data for only one galaxy, but (moderate) flares cannot be ruled out for the other galaxies either. A coplanar ring-like structure is detected outside the main disk of NGC 4217, which we suggest could be the remnant of a recent minor merger event. We also find evidence of a radial inflow of 15 ± 5 km s −1 in the disk of NGC 5529, which might be related to the ongoing interaction with two nearby companions. For NGC 5907, the extended, asymmetric, and strongly warped outer regions of the H  disk also suggest a recent interaction. In contrast, the inner disks of these three galaxies (NGC 4217, NGC 5529, and NGC 5907) show regular behaviour and seem largely unaffected by the interactions. Our models further support earlier claims of prominent spiral arms in the disks of IC 2531 and NGC 5529. Finally, we detect a dwarf companion galaxy at a projected distance of 36 kpc from the centre of NGC 973.

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A Digital Archive of H i 21 Centimeter Line Spectra of Optically Targeted Galaxies

Cited by 472 publications

References 48 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

Structure and dynamics of giant low surface brightness galaxies

HERschelObservations of Edge-on Spirals (HEROES)

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