993 research outputs found
Infrared properties of serendipitous X-ray quasars
Near infrared measurements were obtained of 30 quasars originally found serendipitously as X-ray sources in fields of other objects. The observations show that the infrared characteristics of these quasars do not differ significantly from those of quasars selected by other criteria. Because this X-ray selected sample is subject to different selection biases than previous radio and optical surveys, this conclusion is useful in validating previous inferences regarding the infrared colors of 'typical' quasars
Infrared astronomy research and high altitude observations
Highlights are presented of studies of the emission mechanisms in the 4 to 8 micron region of the spectrum using a circular variable filter wheel spectrometer with a PbSnTe photovoltaic detector. Investigations covered include the spectroscopy of planets, stellar atmospheres, highly obscured objects in molecular clouds, planetary nebulae, H2 regions, and extragalactic objects
Interferometric CO observations of the ultraluminous IRAS galaxies ARP 220, IC 694/NGC 3690, NGC 6420 and NGC 7469
High resolution CO observations of the IRAS galaxies Arp 220, IC 694/NGC 3690, NGC 6240 and NGC 7469 were made with the Millimeter Wave Interferometer of the Owen Valley Radio Observatory. These yield spatial information on scales of 1 to 5 kpc and allow the separation of compact condensations from the more extended emission in the galaxies. In the case of the obviously interacting system IC 694/NGC 3690 the contributions of each component can be discerned. For that galaxy, and also for Arp 220, the unusually high lumonisities may be produced by nonthermal processes rather than by intense bursts of star formation
Black hole in the West Nucleus of Arp 220
We present new observations with the IRAM Interferometer, in its
longest-baseline configuration, of the CO(2-1) line and the 1.3mm dust
radiation from the Arp 220 nuclear region. The dust source in the West nucleus
has a size of 0.19 x 0.13 arcsec and a 1.3mm brightness temperature of 90K.
This implies that the dust ring in the West nucleus has a high opacity, with
tau = 1 at 1.1mm. Not only is the dust ring itself optically thick in the submm
and far-IR, but it is surrounded by the previously-known, rapidly rotating
molecular disk of size 0.5 arcsec that is also optically thick in the mid-IR.
The molecular ring is cooler than the hot dust disk because the CO(2-1) line is
seen in absorption against the dust disk. The dust ring is massive (1E9 solar
masses), compact (radius 35pc), and hot (true dust temperature 170K). It
resembles rather strikingly the dust ring detected around the quasar APM
08279+52, and is most unlike the warm, extended dust sources in starburst
galaxies. Because there is a strong temperature gradient from the hot dust ring
to the cooler molecular disk, the heating must come from a concentrated source,
an AGN accretion disk that is completely invisible at optical wavelengths, and
heavily obscured in hard X-rays.Comment: Reference list updated for 2007 publications; estimated position
errors increase
Construction and evaluation of self-teaching exercises in capitalization and punctuation through team learning in grades four, five, and six.
Thesis (Ed.M.)--Boston Universit
Near Infrared Imaging of the Hubble Deep Field with The Keck Telescope
Two deep K-band () images, with point-source detection limits of
mag (one sigma), taken with the Keck Telescope in subfields of the
Hubble Deep Field, are presented and analyzed. A sample of objects to K=24 mag
is constructed and and colors are measured. By
stacking visually selected objects, mean colors can be measured to
very faint levels; the mean color is constant with apparent
magnitude down to mag.Comment: Replaced with slightly revised source positions and corrected V-I
magnitudes (which were incorrect in the Tables and Figure 5). 18 pages. The
data are publicly available at http://www.cco.caltech.edu/~btsoifer/hdf.html
along with a high-resolution version of Fig.
The IRAS Revised Bright Galaxy Sample (RBGS)
IRAS flux densities, redshifts, and infrared luminosities are reported for
all sources identified in the IRAS Revised Bright Galaxy Sample (RBGS), a
complete flux-limited survey of all extragalactic objects with total 60 micron
flux density greater than 5.24 Jy, covering the entire sky surveyed by IRAS at
Galactic latitude |b| > 5 degrees. The RBGS includes 629 objects, with a median
(mean) sample redshift of 0.0082 (0.0126) and a maximum redshift of 0.0876. The
RBGS supersedes the previous two-part IRAS Bright Galaxy Samples, which were
compiled before the final ("Pass 3") calibration of the IRAS Level 1 Archive in
May 1990. The RBGS also makes use of more accurate and consistent automated
methods to measure the flux of objects with extended emission. Basic properties
of the RBGS sources are summarized, including estimated total infrared
luminosities, as well as updates to cross-identifications with sources from
optical galaxy catalogs established using the NASA/IPAC Extragalactic Database
(NED). In addition, an atlas of images from the Digitized Sky Survey with
overlays of the IRAS position uncertainty ellipse and annotated scale bars is
provided for ease in visualizing the optical morphology in context with the
angular and metric size of each object. The revised bolometric infrared
luminosity function, phi(L_ir), for infrared bright galaxies in the local
Universe remains best fit by a double power law, phi(L_ir) ~ L_ir^alpha, with
alpha = -0.6 (+/- 0.1), and alpha = -2.2 (+/- 0.1) below and above the
"characteristic" infrared luminosity L_ir ~ 10^{10.5} L_solar, respectively.
(Abridged)Comment: Accepted for publication in the Astronomical Journal. Contains 50
pages, 7 tables, 16 figures. Due to astro-ph space limits, only 1 of 26 pages
of Figure 1, and 1 of 11 pages of Table 7, are included; full resolution
Postscript files are available at
http://nedwww.ipac.caltech.edu/level5/March03/IRAS_RBGS/Figures/ .
Replacement: Corrected insertion of Fig. 15 (MethodCodes.ps) in LaTe
The Nature of the Compact/Symmetric Near-IR Continuum Source in 4C 40.36
Using NICMOS on HST, we have imaged the emission-line nebulae and the
line-free continuum in 4C 40.36, a ultra-steep spectrum FR II radio galaxy at
z=2.269. The line-free continuum was found to be extremely compact and
symmetric while the emission-line nebulae seen in H-alpha+[N II] show very
clumpy structures spreading almost linearly over 16 kpc. However, this linear
structure is clearly misaligned from the radio axis. The SED of the line-free
continuum is very flat, suggesting that if the continuum emission is produced
by a single source, it is likely to be a young bursting stellar population or
scattered AGN light. However, because of the lack of a line-free optical image
with a comparable spatial resolution, we cannot exclude the possibility that
the observed SED is a composite of a young blue population and an old red
population.Comment: 4 pages, 2 figures; to appear in the proceedings of "The Hy-Redshift
Universe: Galaxy Formation and Evolution at High Redshift", eds. A.J.Bunker
and W. J. M. van Breuge
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