355 research outputs found
The Optical Polarization Properties of X-ray Selected BL Lacertae Objects
We discuss the optical polarization properties of X-ray selected BL Lacertae
objects (XSBLs) as determined from three years of monitoring 37 BL Lac objects
and candidates. The observed objects include a complete X-ray flux limited
sample drawn from the EMS Survey. The majority of the XSBLs classi- fied solely
on the appearance of their spectra are members of the class of BL~Lacs since
they possess intrinsically polarized and variable continua. The duty cycle of
polarized emission from XSBLs is 40\%. The majority of XSBLs (\%)
have preferred polarization position angles on time scales as long as three
years. This reflects stability in the geometry of the region emitting the
polarized optical emission. We discuss the observed spectral dependence of the
degree of polarization and some of the possible mechanisms for producing the
observed characteristics. While dilution of the polarized emission by the host
galaxy starlight is present in some objects, we demon- strate that the average
polarization properties derived from our observations are not drastically
affected by this effect. The objects in our monitored sample did not display
the larger than one magnitude variations generally used to characterize the
optical variability of blazars in general.Comment: LaTex file, 21 pages, with tables appended as a poscript file.
Contact [email protected] for postscript figure files. Institute for Advanced
Study number AST 93/4
The Spectral Energy Distribution and Infrared Luminosities of z ≈ 2 Dust-obscured Galaxies from Herschel and Spitzer
Dust-obscured galaxies (DOGs) are a subset of high-redshift (z ≈ 2) optically-faint ultra-luminous infrared galaxies (ULIRGs, e.g., L_(IR) > 10^(12) L_☉). We present new far-infrared photometry, at 250, 350, and 500 μm (observed-frame), from the Herschel Space Telescope for a large sample of 113 DOGs with spectroscopically measured redshifts. Approximately 60% of the sample are detected in the far-IR. The Herschel photometry allows the first robust determinations of the total infrared luminosities of a large sample of DOGs, confirming their high IR luminosities, which range from 10^(11.6) L_☉ 10^(13) L_☉. The rest-frame near-IR (1-3 μm) spectral energy distributions (SEDs) of the Herschel-detected DOGs are predictors of their SEDs at longer wavelengths. DOGs with "power-law" SEDs in the rest-frame near-IR show observed-frame 250/24 μm flux density ratios similar to the QSO-like local ULIRG, Mrk 231. DOGs with a stellar "bump" in their rest-frame near-IR show observed-frame 250/24 μm flux density ratios similar to local star-bursting ULIRGs like NGC 6240. None show 250/24 μm flux density ratios similar to extreme local ULIRG, Arp 220; though three show 350/24 μm flux density ratios similar to Arp 220. For the Herschel-detected DOGs, accurate estimates (within ~25%) of total IR luminosity can be predicted from their rest-frame mid-IR data alone (e.g., from Spitzer observed-frame 24 μm luminosities). Herschel-detected DOGs tend to have a high ratio of infrared luminosity to rest-frame 8 μm luminosity (the IR8 = L_(IR)(8-1000 μm)/νL_ν(8 μm) parameter of Elbaz et al.). Instead of lying on the z = 1-2 "infrared main sequence" of star-forming galaxies (like typical LIRGs and ULIRGs at those epochs) the DOGs, especially large fractions of the bump sources, tend to lie in the starburst sequence. While, Herschel-detected DOGs are similar to scaled up versions of local ULIRGs in terms of 250/24 μm flux density ratio, and IR8, they tend to have cooler far-IR dust temperatures (20-40 K for DOGs versus 40-50 K for local ULIRGs) as measured by the rest-frame 80/115 μm flux density ratios (e.g., observed-frame 250/350 μm ratios at z = 2). DOGs that are not detected by Herschel appear to have lower observed-frame 250/24 μm ratios than the detected sample, either because of warmer dust temperatures, lower IR luminosities, or both
Detection of Extended Polarized Ultraviolet Radiation from the z = 1.82 Radio Galaxy 3C 256
We have detected spatially extended linear polarized UV emission from the
high-redshift radio galaxy 3C~256 (). A spatially integrated (
diameter aperture) measurement of the degree of polarization of the band
(rest frame 0.19 m) emission yields a value of 16.4\% (\%) with a
position angle of (),
orthogonal to the position angle on the sky of the major axis of the extended
emission. The peak emission measured with a diameter circular aperture
is 11.7\% (\%) polarized with a position angle of (). An image of the polarized flux is
presented, clearly displaying that the polarized flux is extended and present
over the entire extent of the object. While it has been suggested that the UV
continuum of 3C~256 might be due to star formation (Elston 1988) or a
protogalaxy (Eisenhardt \& Dickinson 1993) based on its extremely blue spectral
energy distribution and similar morphology at UV and visible wavelengths, we
are unable to reconcile the observed high degree of polarization with such a
model. While the detection of polarized emission from HZRGs has been shown to
be a common phenomena, 3C~256 is only the third object for which a measurement
of the extended polarized UV emission has been presented. These data lend
additional support to the suggestion first made by di Serego Alighieri and
collaborators that the ``alignment effect'', the tendency for the extended UV
continuum radiation and line emission from HZRGs to be aligned with the major
axis of the extended radio emission, is in large part due to scattering of
anisotropic nuclear emission.Comment: 11 pages, LaTeX (aaspp style) file. Figure available by request to
[email protected]
High-Redshift Dust Obscured Galaxies: A Morphology-Spectral Energy Distribution Connection Revealed by Keck Adaptive Optics
A simple optical to mid-IR color selection, R – [24]>14, i.e., f_ν(24 μm)/f_ν(R) ≳ 1000, identifies highly dust obscured galaxies (DOGs) with typical redshifts of z ~ 2 ± 0.5. Extreme mid-IR luminosities (L_(IR) > 10^(12-14)) suggest that DOGs are powered by a combination of active galactic nuclei (AGNs) and star formation, possibly driven by mergers. In an effort to compare their photometric properties with their rest-frame optical morphologies, we obtained high-spatial resolution (0."05-0."1) Keck Adaptive Optics K'-band images of 15 DOGs. The images reveal a wide range of morphologies, including small exponential disks (eight of 15), small ellipticals (four of 15), and unresolved sources (two of 15). One particularly diffuse source could not be classified because of low signal-to-noise ratio. We find a statistically significant correlation between galaxy concentration and mid-IR luminosity, with the most luminous DOGs exhibiting higher concentration and smaller physical size. DOGs with high concentration also tend to have spectral energy distributions (SEDs) suggestive of AGN activity. Thus, central AGN light may be biasing the morphologies of the more luminous DOGs to higher concentration. Conversely, more diffuse DOGs tend to show an SED shape suggestive of star formation. Two of 15 in the sample show multiple resolved components with separations of ~1 kpc, circumstantial evidence for ongoing mergers
The Star Formation Histories of z ~ 2 Dust-obscured Galaxies and Submillimeter-selected Galaxies
The Spitzer Space Telescope has identified a population of ultraluminous infrared galaxies (ULIRGs) at z ~ 2 that may play an important role in the evolution of massive galaxies. We measure the stellar masses (M_*) of two populations of Spitzer-selected ULIRGs that have extremely red R – [24] colors (dust-obscured galaxies, or DOGs) and compare our results with submillimeter-selected galaxies (SMGs). One set of 39 DOGs has a local maximum in their mid-infrared (mid-IR) spectral energy distribution (SED) at rest frame 1.6 μm associated with stellar emission ("bump DOGs"), while the other set of 51 DOGs have power-law mid-IR SEDs that are typical of obscured active galactic nuclei ("power-law DOGs"). We measure M_* by applying Charlot & Bruzual stellar population synthesis models to broadband photometry in the rest-frame ultraviolet, optical, and near-infrared of each of these populations. Assuming a simple stellar population and a Chabrier initial mass function, we find that power-law DOGs and bump DOGs are on average a factor of 2 and 1.5 more massive than SMGs, respectively (median and inter-quartile M_* values for SMGs, bump DOGs, and power-law DOGs are log(M_*/M_☉) = 10.42^(+0.42)_(–0.36), 10.62^(+0.36)_(–0.32), and 10.71^(+0.40)_(–0.34), respectively). More realistic star formation histories drawn from two competing theories for the nature of ULIRGs at z ~ 2 (major merger versus smooth accretion) can increase these mass estimates by up to 0.5 dex. A comparison of our stellar masses with the instantaneous star formation rate (SFR) in these z ~ 2 ULIRGs provides a preliminary indication supporting high SFRs for a given M_*, a situation that arises more naturally in major mergers than in smooth accretion-powered systems
Morphologies of High Redshift, Dust Obscured Galaxies from Keck Laser Guide Star Adaptive Optics
Spitzer MIPS images in the Bootes field of the NOAO Deep Wide-Field Survey
have revealed a class of extremely dust obscured galaxy (DOG) at z~2. The DOGs
are defined by very red optical to mid-IR (observed-frame) colors, R - [24 um]
> 14 mag, i.e. f_v (24 um) / f_v (R) > 1000. They are Ultra-Luminous Infrared
Galaxies with L_8-1000 um > 10^12 -10^14 L_sun, but typically have very faint
optical (rest-frame UV) fluxes. We imaged three DOGs with the Keck Laser Guide
Star Adaptive Optics (LGSAO) system, obtaining ~0.06'' resolution in the
K'-band. One system was dominated by a point source, while the other two were
clearly resolved. Of the resolved sources, one can be modeled as a exponential
disk system. The other is consistent with a de Vaucouleurs profile typical of
elliptical galaxies. The non-parametric measures of their concentration and
asymmetry, show the DOGs to be both compact and smooth. The AO images rule out
double nuclei with separations of greater than 0.1'' (< 1 kpc at z=2), making
it unlikely that ongoing major mergers (mass ratios of 1/3 and greater) are
triggering the high IR luminosities. By contrast, high resolution images of z~2
SCUBA sources tend to show multiple components and a higher degree of
asymmetry. We compare near-IR morphologies of the DOGs with a set of z=1
luminous infrared galaxies (LIRGs; L_IR ~ 10^11 L_sun) imaged with Keck LGSAO
by the Center for Adaptive Optics Treasury Survey. The DOGs in our sample have
significantly smaller effective radii, ~1/4 the size of the z=1 LIRGs, and tend
towards higher concentrations. The small sizes and high concentrations may help
explain the globally obscured rest-frame blue-to-UV emission of the DOGs.Comment: 9 pages, 7 figures, 2 tables, accepted for publication in the
Astronomical Journa
The Compact X-ray Source 1E 1547.0-5408 and the Radio Shell G327.24-0.13: A New Proposed Association between a Candidate Magnetar and a Candidate Supernova Remnant
We present X-ray, infrared and radio observations of the field centered on
X-ray source 1E 1547.0-5408 in the Galactic Plane. A new Chandra observation of
this source shows it is unresolved at arc-second resolution, and a new XMM
observation shows that its X-ray spectrum is best described by an absorbed
power-law and blackbody model. A comparison of the X-ray flux observed from
this source between 1980 and 2006 reveals that its absorbed 0.5-10 keV X-ray
flux decreased from ~2x10^-12 ergs cm-2 s-1 to ~3x10^-13 ergs cm-2 during this
period. The most recent XMM observation allows us to put a 5 sigma confidence
upper limit of 14% for the 0.5-10 keV peak-to-peak pulsed fraction. A
near-infrared observation of this field shows a source with magnitude Ks =
15.9+/-0.2 near the position of 1E 1547.0-5408, but the implied X-ray to
infrared flux ratio indicates the infrared emission is from an unrelated field
source, allowing us to limit the IR magnitude of 1E 1547.0-5408 to >17.5.
Archival radio observations reveal that 1E 1547.0-5408 sits at the center of a
faint, small (4' diameter) radio shell, G327.24-0.13, which is possibly a
previously unidentified supernova remnant. The X-ray properties of 1E
1547.0-5408 suggest that this source is a magnetar - a young neutron star whose
X-ray emission is powered by the decay of its extremely strong magnetic field.
The spatial coincidence between this source and G327.24-0.13 suggests that 1E
1547.0-5408 is associated with a young supernova remnant, supporting a neutron
star interpretation. Additional observations are needed to confirm the nature
of both 1E 1547.0-5408 and G327.24-0.13, and to determine if these sources are
associated. If so, this pair will be an important addition to the small number
of known associations between magnetars and supernova remnants.Comment: 11 pages, 5 figures, ApJ accepte
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