Fri, Nov 30

Kinematics and Excitation of the Molecular Hydrogen Accretion Disc in NGC 1275

J. Scharwaechter, P. J. McGregor, M. A. Dopita, T. L. Beck
(Submitted on 28 Nov 2012)

We report the results of high spatial and spectral resolution integral-field spectroscopy of the central ~3 x 3 arcsec^2 of the active galaxy NGC 1275 (Perseus A), based on observations with the Near-infrared Integral Field Spectrograph (NIFS) and the ALTAIR adaptive-optics system on the Gemini North telescope. The circum-nuclear disc in the inner R~50 pc of NGC 1275 is seen in both the H2 and [FeII] lines. The disc is interpreted as the outer part of a collisionally-excited turbulent accretion disc. The kinematic major axis of the disc at a position angle of 68 deg is oriented perpendicular to the radio jet. A streamer-like feature to the south-west of the disc, detected in H2 but not in [FeII], is discussed as one of possibly several molecular streamers, presumably falling into the nuclear region. Indications of an ionization structure within the disc are deduced from the HeI and Br gamma emission lines, which may partially originate from the inner portions of the accretion disc. The kinematics of these two lines agrees with the signature of the circum-nuclear disc, but both lines display a larger central velocity dispersion than the H2 line. The rovibrational H2 transitions from the core of NGC 1275 are indicative of thermal excitation caused by shocks and agree with excitation temperatures of ~1360 and ~4290 K for the lower- and higher-energy H2 transitions, respectively. The data suggest X-ray heating as the dominant excitation mechanism of [FeII] emission in the core, while fast shocks are a possible alternative. The [FeII] lines indicate an electron density of ~4000 cm^{-3}. The H2 disc is modelled using simulated NIFS data cubes of H2 emission from inclined discs in Keplerian rotation around a central mass. Assuming a disc inclination of 45 deg +/- 10 deg, the best-fitting models imply a central mass of (8^{+7}_{-2}) x 10^8 Msun. (abridged)

Comments: 19 pages, 17 figures, 1 table, accepted for publication in MNRAS
Subjects: Cosmology and Extragalactic Astrophysics (astro-ph.CO); Galaxy Astrophysics (astro-ph.GA)
Cite as: arXiv:1211.6750 [astro-ph.CO]
(or arXiv:1211.6750v1 [astro-ph.CO] for this version)

The anatomy of an extreme starburst within 1.3Gyr of the Big Bang revealed by ALMA

C.L. Carilli (NRAO), D. Riechers (Cornell), F. Walter (MPIA), R. Maiolino (MRAO), J. Wagg (ESO), L. Lentati (MRAO), R. McMahon (IoA), W. Wolfe (UCSD)
(Submitted on 29 Nov 2012)

We present further analysis of the [CII] 158$\mu$m fine structure line and thermal dust continuum emission from the archetype extreme starburst/AGN group of galaxies in the early Universe, BRI 1202-0725 at $z=4.7$, using the Atacama Large Millimeter Array. The group is long noted for having a closely separated (26kpc in projection) FIR-hyperluminous quasar host galaxy and an optically obscured submm galaxy (SMG). A short ALMA test observation reveals a rich laboratory for the study of the myriad processes involved in clustered massive galaxy formation in the early Universe. Strong [CII] emission from the SMG and the quasar have been reported earlier by Wagg et al. (2012) based on these observations. In this letter, we examine in more detail the imaging results from the ALMA observations, including velocity channel images, position-velocity plots, and line moment images. We present detections of [CII] emission from two Ly$\alpha$-selected galaxies in the group, demonstrating the relative ease with which ALMA can detect the [CII] emission from lower star formation rate galaxies at high redshift. Imaging of the [CII] emission shows a clear velocity gradient across the SMG, possibly indicating rotation or a more complex dynamical system on a scale $\sim 10$kpc. There is evidence in the quasar spectrum and images for a possible outflow toward the southwest, as well as more extended emission (a ‘bridge’), between the quasar and the SMG, although the latter could simply be emission from Ly$\alpha$-1 blending with that of the quasar at the limited spatial resolution of the current observations. These results provide an unprecedented view of a major merger of gas rich galaxies driving extreme starbursts and AGN accretion during the formation of massive galaxies and supermassive black holes within 1.3 Gyr of the Big Bang.

Comments: for the astrophysical journal. 5 figs
Subjects: Cosmology and Extragalactic Astrophysics (astro-ph.CO)
Cite as: arXiv:1211.6973 [astro-ph.CO]
(or arXiv:1211.6973v1 [astro-ph.CO] for this version)

A High Resolution Study of the Atomic Hydrogen in CO-Rich Early-Type Galaxies

Danielle M. Lucero, Lisa M. Young
(Submitted on 29 Nov 2012)

We present an analysis of new and archival VLA HI observations of a sample of eleven early-type galaxies rich in CO, with detailed comparisons of CO and HI distributions and kinematics. The early-type sample consists of both lenticular and elliptical galaxies in a variety of environments. A range of morphologies and environments were selected in order to give a broader understanding of the origins, distribution, and fate of the cold gas in early-type galaxies. Six of the eleven galaxies in the sample are detected in both HI and CO. The H$_{2}$ to HI mass ratios for this sample range from 0.2-120. The HI morphologies of the sample are consistent with that of recent HI surveys of early-type galaxies which also find a mix of HI morphologies and masses, low HI peak surface densities, and a lack of HI in early-type galaxies which reside in high density environments. The HI-detected galaxies have a wide range of HI masses (1.4$\times10^{6}$ to 1.1$\times10^{10}$ M$_{\odot}$). There does not appear to be any correlation between the HI mass and morphology (E versus S0). When HI is detected, it is centrally peaked – there are no central kpc-scale central HI depressions like those observed for early-type spiral galaxies at similar spatial resolutions and scales. A kinematic comparison between the HI and CO indicates that both cold gas components share the same origin. The primary goal of this and a series of future papers is to better understand the relationship between the atomic and molecular gas in early-type galaxies, and to compare the observed relationships with those of spiral galaxies where this relationship has been studied in depth.

Comments: 35 pages, 26 figures, Accepted to AJ. I have used emulateapj to make the article resemble how it may appear in the actual Journal. The result is not perfect, but will take up less paper and will hopefully be easier for you all to read
Subjects: Galaxy Astrophysics (astro-ph.GA)
Cite as: arXiv:1211.6808 [astro-ph.GA]
(or arXiv:1211.6808v1 [astro-ph.GA] for this version)
Advertisements
This entry was posted in Uncategorized. Bookmark the permalink.

Leave a Reply

Fill in your details below or click an icon to log in:

WordPress.com Logo

You are commenting using your WordPress.com account. Log Out / Change )

Twitter picture

You are commenting using your Twitter account. Log Out / Change )

Facebook photo

You are commenting using your Facebook account. Log Out / Change )

Google+ photo

You are commenting using your Google+ account. Log Out / Change )

Connecting to %s