اشترك بالحزمة الذهبية واحصل على وصول غير محدود شمرا أكاديميا
تسجيل مستخدم جديدAMI Galactic Plane Survey at 16 GHz: I -- Observing, mapping and source extraction
126
0
0.0
(
0
)
اسأل ChatGPT حول البحث
ﻻ يوجد ملخص باللغة العربية
The AMI Galactic Plane Survey (AMIGPS) is a large area survey of the outer Galactic plane to provide arcminute resolution images at milli-Jansky sensitivity in the centimetre-wave band. Here we present the first data release of the survey, consisting of 868 deg^2 of the Galactic plane, covering the area 76 deg lessapprox l lessapprox 170 deg between latitudes of |b| lessapprox 5 deg, at a central frequency of 15.75 GHz (1.9 cm). We describe in detail the drift scan observations which have been used to construct the maps, including the techniques used for observing, mapping and source extraction, and summarise the properties of the finalized datasets. These observations constitute the most sensitive Galactic plane survey of large extent at centimetre-wave frequencies greater than 1.4 GHz.
قيم البحث
اقرأ أيضاً
The H.E.S.S. Galactic Plane Survey (HGPS), the first comprehensive survey of the inner Galaxy at TeV energies, has led to the discovery of an unexpectedly large and diverse population of over 60 sources of TeV gamma rays within its current range of l
= 250 to 65 degrees in longitude and |b| < 3.5 degrees in latitude. The data set of the HGPS comprises 2800 hours of high-quality data, taken in the years 2004 to 2013. The sensitivity for the detection of point-like sources is at the level of 2% Crab or better in the HGPS region. The population of TeV gamma-ray emitters is dominated by the pulsar wind nebula and supernova remnant source classes, although nearly a third of the sources remain unidentified or ambiguous. We are presenting the latest HGPS significance and sensitivity maps, as well as a work on the HGPS source catalog, based on a uniform re-analysis of the full data set collected in the last decade. We will also give a brief overview of the H.E.S.S. Galactic source population.
The Planck Early Release Compact Source Catalogue includes 26 sources with no obvious matches in other radio catalogues (of primarily extragalactic sources). Here we present observations made with the Arcminute Microkelvin Imager Small Array (AMI SA)
at 15.75 GHz of the eight of the unmatched sources at declination > +10 degrees. Of the eight, four are detected and are associated with known objects. The other four are not detected with the AMI SA, and are thought to be spurious.
We investigate the serendipitous X-ray source population revealed in XMM-Newton observations targeted in the Galactic Plane within the region 315<l<45 and |b|<2.5 deg. Our study focuses on a sample of 2204 X-ray sources at intermediate to faint fluxe
s, which were detected in a total of 116 XMM fields and are listed in the 2XMMi catalogue. We characterise each source as spectrally soft or hard on the basis of whether the bulk of the recorded counts have energies below or above 2 keV and find that the sample divides roughly equally (56%:44%) into these soft and hard categories. The X-ray spectral form underlying the soft sources may be represented as either a power-law continuum with Gamma~2.5 or a thermal spectrum with kT~0.5 keV, with N_H ranging from 10^{20-22} cm^{-2}. For the hard sources, a significantly harder continuum form is likely, i.e., Gamma~1 with N_H=10^{22-24} cm^{-2}. For ~50% of the hard sources, the inferred column density is commensurate with the total Galactic line-of-sight value; many of these sources will be located at significant distances across the Galaxy implying a hard band luminosity L_X>10^{32} erg/s, whereas some will be extragalactic interlopers. >90% of the soft sources have potential NIR (2MASS and/or UKIDSS) counterparts inside their error circles, consistent with the dominant soft X-ray source population being relatively nearby coronally-active stars. These stellar counterparts are generally brighter than J=16, a brightness cutoff which corresponds to the saturation of the X-ray coronal emission at L_X=10^{-3} L_{bol}. In contrast, the success rate in finding likely IR counterparts to the hard X-ray sample is no more than ~15% down to J=16 and ~25% down to J=20, set against a rapidly rising chance coincidence rate. The make-up of the hard X-ray source population, in terms of the known classes of accreting and non-accreting systems, remains uncertain.
We present a proper motion survey of the Galactic plane, using IPHAS data and POSS-I Schmidt plate data as a first epoch, that probes down to proper motions below 50 milliarcseconds per year. The IPHAS survey covers the northern plane ($|b| < 5^{circ
}$) with CCD photometry in the $r$, $i$ and H${alpha}$ passbands. We examine roughly 1400 sq. deg. of the IPHAS survey area and draw up a catalogue containing 103058 objects with significant proper motions below 150 millarcseconds per year in the magnitude range 13.5$< r <$19. Our survey sample contains large samples of white dwarfs and subdwarfs which can be identified using a reduced proper motion diagram. We also found several objects with IPHAS colours suggesting H${alpha}$ emission and significant proper motions. One is the known cataclysmic variable GD552; two are known DB white dwarfs and five others are found to be non-DA (DB and DC) white dwarfs, which were included in the H$alpha$ emission line catalogue due to their lack of absorption in the H$alpha$ narrow-band.
The Very Large Array Sky Survey (VLASS) is observing the entire sky north of $-40^{circ}$ in the S-band ($2< u<4,$GHz), with the highest angular resolution ($2.5$) of any all-sky radio continuum survey to date. VLASS will cover its entire footprint o
ver three distinct epochs, the first of which has now been observed in full. Based on Quick Look images from this first epoch, we have created a catalog of $1.9times10^{6}$ reliably detected radio components. Due to the limitations of the Quick Look images, component flux densities are underestimated by $sim 15,%$ at $S_{text{peak}}>3,$mJy/beam and are often unreliable for fainter components. We use this catalog to perform statistical analyses of the $ u sim 3,$GHz radio sky. Comparisons with the Faint Images of the Radio Sky at Twenty cm survey (FIRST) show the typical $1.4-3,$GHz spectral index, $alpha$, to be $sim-0.71$. The radio color-color distribution of point and extended components is explored by matching with FIRST and the LOFAR Two Meter Sky Survey. We present the VLASS source counts, $dN/dS$, which are found to be consistent with previous observations at $1.4$ and $3,$GHz. Resolution improvements over FIRST result in excess power in the VLASS two-point correlation function at angular scales $lesssim 7$, and in $18,%$ of active galactic nuclei associated with a single FIRST component being split into multi-component sources by VLASS.
سجل دخول لتتمكن من نشر تعليقات
التعليقات
جاري جلب التعليقات
سجل دخول لتتمكن من متابعة معايير البحث التي قمت باختيارها
