- ID:
- ivo://CDS.VizieR/J/MNRAS/429/3330
- Title:
- AMI Galactic Plane Survey at 16GHz. I.
- Short Name:
- J/MNRAS/429/3330
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The AMI Galactic Plane survey is being made with the Arcminute Microkelvin Imager (AMI) Small Array at 15.7GHz and with resolution of approximately 3arcmin. This is the first data release, covering ~868deg^2^ of the Northern Galactic plane between |b|~+/-5{deg} and above {delta}=40{deg} with a noise level of ~3mJy/beam away from bright sources. The source catalogue contains a total of 3503 sources.
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Search Results
- ID:
- ivo://CDS.VizieR/J/MNRAS/453/1396
- Title:
- AMI Galactic Plane Survey at 16GHz. II.
- Short Name:
- J/MNRAS/453/1396
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Arcminute Microkelvin Imager Galactic Plane Survey (AMIGPS) provides mJy-sensitivity, arcminute-resolution interferometric images of the northern Galactic plane at ~16GHz. The first data release covered 76{deg}<=l<=170{deg} between latitudes of |b|<=5{deg}; here we present a second data release, extending the coverage to 53{deg}<=l<=193{deg} and including high-latitude extensions to cover the Taurus and California giant molecular cloud regions, and the recently discovered large supernova remnant G159.6+7.3. The total coverage is now 1777{deg}^2^ and the catalogue contains 6509 sources. We also describe the improvements to the data processing pipeline which improves the positional and flux density accuracies of the survey.
- ID:
- ivo://CDS.VizieR/VIII/86
- Title:
- Analysis of the RC catalog sample.
- Short Name:
- VIII/86
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- of paper I: 432 radio sources of the RC catalog produced in 1980-1985 at RATAN-600 radio telescope based on a deep survey of a sky strip centered on the declination of the SS433 source are identified in the region overlapping with FIRST and SDSS surveys (about 132{deg}^2^ large). The NVSS catalog was used as the reference catalog for refining the coordinates of the radio sources. The morphology is found for about 75% of the objects of the sample and the ratio of single, double and multicomponent radio sources is computed based on FIRST radio maps. The 74, 365, 1400, and 4850MHz data of the VLSS, TXS, NVSS, FIRST, and GB6 catalogs are used to analyze the shape of the spectra.
- ID:
- ivo://CDS.VizieR/J/ApJS/241/37
- Title:
- 1.4 and 5GHz deep JVLA radio survey of M33
- Short Name:
- J/ApJS/241/37
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have performed new 1.4 and 5 GHz observations of the Local Group galaxy M33 with the Jansky Very Large Array. Our survey has a limiting sensitivity of 20{mu}Jy (4{sigma}) and a resolution of 5.9" (FWHM), corresponding to a spatial resolution of 24pc at 817kpc. Using a new multiresolution algorithm, we have created a catalog of 2875 sources, including 675 with well-determined spectral indices. We detect sources at the position of 319 of the X-ray sources in the Tullmann+ (2011, J/ApJS/193/31) Chandra survey of M33, the majority of which are likely to be background galaxies. The radio source coincident with M33 X-8, the nuclear source, appears to be extended. Along with numerous HII regions or portions of HII region complexes, we detect 155 of the 217 optical supernova remnants (SNRs) included in the lists of Long+, 2010, J/ApJS/187/495 and Lee & Lee, 2014, J/ApJ/793/134, making this by far the largest sample of remnants at known distances with multiwavelength coverage. The remnants show a large dispersion in the ratio of radio to X-ray luminosity at a given diameter, a result that challenges the current generation of models for synchrotron radiation evolution in SNRs.
- ID:
- ivo://CDS.VizieR/J/AJ/119/2801
- Title:
- 8.35 and 14.35GHz flux at Galactic plane
- Short Name:
- J/AJ/119/2801
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the first images of the Galactic plane (GP; |b|<5{deg}, -15{deg}<l<255{deg}) at 8.35 and 14.35 GHz. These observations used the National Radio Astronomy Observatory-NASA Green Bank Earth Station to survey the sky simultaneously at these frequencies. These are the first results from the GP survey observations, a program to monitor the sky at 8.35 and 14.35 GHz. The GP survey series is intended to detect short-lived radio sources. We present four independent observations of the Galactic plane, combined to provide a set of reference images of the Galactic plane. The first survey, GPA, covers 0.82 sr (6.5%) of the sky. A source list is presented for all sources brighter than 0.9 Jy at 8.35 GHz and also for all sources brighter than 2.5 Jy at 14.35 GHz. The FITS format images, residual images, source lists, and archive data are available over the Internet. Later papers will present the results of the variable source search.
- ID:
- ivo://CDS.VizieR/J/A+A/565/A103
- Title:
- Anomalous microwave emission in Galactic clouds
- Short Name:
- J/A+A/565/A103
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Anomalous microwave emission (AME) is believed to be due to electric dipole radiation from small spinning dust grains. The aim of this paper is a statistical study of the basic properties of AME regions and the environment in which they emit. We used WMAP and Planck maps, combined with ancillary radio and IR data, to construct a sample of 98 candidate AME sources, assembling SEDs for each source using aperture photometry on 1{deg}-smoothed maps from 0.408GHz up to 3000GHz. Each spectrum is fitted with a simple model of free-free, synchrotron (where necessary), cosmic microwave background (CMB), thermal dust, and spinning dust components. We find that 42 of the 98 sources have significant (>5{sigma}) excess emission at frequencies between 20 and 60GHz. An analysis of the potential contribution of optically thick free-free emission from ultra-compact HII regions, using IR colour criteria, reduces the significant AME sample to 27 regions. The spectrum of the AME is consistent with model spectra of spinning dust. Peak frequencies are in the range 20-35GHz except for the California nebula (NGC1499), which appears to have a high spinning dust peak frequency of (50+/-17)GHz. The AME regions tend to be more spatially extended than regions with little or no AME. The AME intensity is strongly correlated with the sub-millimetre/IR flux densities and comparable to previous AME detections in the literature. AME emissivity, defined as the ratio of AME to dust optical depth, varies by an order of magnitude for the AME regions. The AME regions tend to be associated with cooler dust in the range 14-20K and an average emissivity index, {beta}_d_, of +1.8, while the non-AME regions are typically warmer, at 20-27K. In agreement with previous studies, the AME emissivity appears to decrease with increasing column density. This supports the idea of AME originating from small grains that are known to be depleted in dense regions, probably due to coagulation onto larger grains. We also find a correlation between the AME emissivity (and to a lesser degree the spinning dust peak frequency) and the intensity of the interstellar radiation field, G_0_. Modelling of this trend suggests that both radiative and collisional excitation are important for the spinning dust emission. The most significant AME regions tend to have relatively less ionized gas (free-free emission), although this could be a selection effect. The infrared excess, a measure of the heating of dust associated with HII regions, is typically >4 for AME sources, indicating that the dust is not primarily heated by hot OB stars. The AME regions are associated with known dark nebulae and have higher 12{mu}m/25{mu}m ratios. The emerging picture is that the bulk of the AME is coming from the polycyclic aromatic hydrocarbons and small dust grains from the colder neutral interstellar medium phase.
- ID:
- ivo://CDS.VizieR/J/ApJ/812/81
- Title:
- Arecibo Pulsar-ALFA (PALFA) survey. IV.
- Short Name:
- J/ApJ/812/81
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The on-going Arecibo Pulsar-ALFA (PALFA) survey began in 2004 and is searching for radio pulsars in the Galactic plane at 1.4GHz. Here we present a comprehensive description of one of its main data reduction pipelines that is based on the PRESTO software and includes new interference-excision algorithms and candidate selection heuristics. This pipeline has been used to discover 40 pulsars, bringing the survey's discovery total to 144 pulsars. Of the new discoveries, eight are millisecond pulsars (MSPs; P<10ms) and one is a Fast Radio Burst (FRB). This pipeline has also re-detected 188 previously known pulsars, 60 of them previously discovered by the other PALFA pipelines. We present a novel method for determining the survey sensitivity that accurately takes into account the effects of interference and red noise: we inject synthetic pulsar signals with various parameters into real survey observations and then attempt to recover them with our pipeline. We find that the PALFA survey achieves the sensitivity to MSPs predicted by theoretical models but suffers a degradation for P>~100ms that gradually becomes up to ~10 times worse for P>4s at DM<150pc/cm^3^. We estimate 33+/-3% of the slower pulsars are missed, largely due to red noise. A population synthesis analysis using the sensitivity limits we measured suggests the PALFA survey should have found 224+/-16 un-recycled pulsars in the data set analyzed, in agreement with the 241 actually detected. The reduced sensitivity could have implications on estimates of the number of long-period pulsars in the Galaxy.
- ID:
- ivo://CDS.VizieR/J/A+A/610/A24
- Title:
- AS 209 ALMA image
- Short Name:
- J/A+A/610/A24
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This paper presents new high angular resolution ALMA 1.3mm dust continuum observations of the protoplanetary system AS 209 in the Ophiuchus star forming region. The dust continuum emission is characterized by a main central core and two prominent rings at r=75au and r=130au intervaled by two gaps at at r=62au and r=103au. The two gaps have different widths and depths, with the inner one being narrower and shallower. We determined the surface density of the millimeter dust grains using the 3D radiative transfer disk code dali. According to our fiducial model the inner gap is partially filled with millimeter grains while the outer gap is largely devoid of dust. The inferred surface density is compared to 3D hydrodynamical simulations (FARGO-3D) of planet-disk interaction. The outer dust gap is consistent with the presence of a giant planet (M_planet_~0.8M_Saturn_); the planet is responsible for the gap opening and for the pile-up of dust at the outer edge of the planet orbit. The simulations also show that the same planet could be the origin of the inner gap at r=62au. The relative position of the two dust gaps is close to the 2:1 resonance and we have investigated the possibility of a second planet inside the inner gap. The resulting surface density (including location, width and depth of the two dust gaps) are in agreement with the observations. The properties of the inner gap pose a strong constraint to the mass of the inner planet (M_planet_<0.1M_J_). In both scenarios (single or pair of planets), the hydrodynamical simulations suggest a very low disk viscosity ({alpha}<10^-4^). Given the young age of the system (0.5-1Myr), this result implies that the formation of giant planets occurs on a timescale of <~1Myr.
- ID:
- ivo://CDS.VizieR/J/MNRAS/506/3540
- Title:
- ASKAP-EMU ESP LMC Radio Continuum Survey
- Short Name:
- J/MNRAS/506/3540
- Date:
- 17 Jan 2022 11:54:41
- Publisher:
- CDS
- Description:
- We present an analysis of a new 120 deg^2^ radio continuum image of the Large Magellanic Cloud (LMC) at 888MHz with a bandwidth of 288MHz and beam size of 13.9"x12.1", from the Australian Square Kilometre Array Pathfinder (ASKAP) processed as part of the Evolutionary Map of the Universe (EMU) survey. The median Root Mean Squared noise is 58uJy/beam. We present a catalogue of 54612 sources, divided over a Gold list (30866 sources) complete down to 0.5mJy uniformly across the field, a Silver list (22080 sources) reaching down to <0.2mJy and a Bronze list (1666 sources) of visually inspected sources in areas of high noise and/or near bright complex emission. We discuss detections of planetary nebulae and their radio luminosity function, young stellar objects showing a correlation between radio luminosity and gas temperature, novae and X-ray binaries in the LMC, and active stars in the Galactic foreground that may become a significant population below this flux level. We present examples of diffuse emission in the LMC (HII regions, supernova remnants, bubbles) and distant galaxies showcasing spectacular interaction between jets and intracluster medium. Among 14333 infrared counterparts of the predominantly background radio source population we find that star-forming galaxies become more prominent below 3mJy compared to active galactic nuclei.We combine the new 888MHz data with archival Australia Telescope Compact Array data at 1.4GHz to determine spectral indices; the vast majority display synchrotron emission but flatter spectra occur too. We argue that the most extreme spectral index values are due to variability.
- ID:
- ivo://CDS.VizieR/J/MNRAS/452/3969
- Title:
- ATCA Survey of Sagittarius B2 at 7mm
- Short Name:
- J/MNRAS/452/3969
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a 30-50GHz survey of Sagittarius B2(N) conducted with the Australia Telescope Compact Array (ATCA) with 5 - 10 arcsec resolution. We analyze the spectra towards three HII regions that have foreground molecular gas in Sgr B2. Towards the most line-dense region, we detect >500 spectral line components, >90% of which are assigned to H and He recombination lines and 53 firmly identified molecular species (not including isotopologues). The data reveal extremely subthermally excited molecular gas in Sgr B2 absorbing against the continuum background, as well as molecular line emission from two hot cores in Sgr B2(N). They also also contain line-of-sight absorption by ~15 molecules observed in translucent gas in the Galactic Center, bar, and intervening spiral arm clouds, revealing the complex chemistry and clumpy structure of this gas. Formamide (NH_2_CHO) is detected for the first time in a translucent cloud.