- ID:
- ivo://nasa.heasarc/wmapitnpts
- Title:
- WMAP 7-Year Internal Templates and Needlets New Source Catalog
- Short Name:
- WMAPITNPTS
- Date:
- 18 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The authors have developed a new needlet-based method to detect point sources in cosmic microwave background (CMB) maps and have applied it to the Wilkinson Microwave Anisotropy Probe (WMAP) 7-year data. They use both the individual frequency channels as well as internal templates, the latter being the difference between pairs of frequency channels and hence having the advantage that the CMB component is eliminated. Using the area of the sky outside the Kq85 galactic mask, they detect a total of 2102 point sources at the 5-sigma level in either the frequency maps or the internal templates. Of these, 1116 are detected either at 5 sigma directly in the frequency channels or at 5 sigma in the internal templates and >= 3 sigma at the corresponding position in the frequency channels. Of the 1116 sources, 603 are detections that have not been reported so far in WMAP data. The authors have made a catalog of these sources available with position and flux estimated in the WMAP channels where they are seen. In total, they identified 1029 of the 1116 sources with counterparts at 5 GHz and 69 at other frequencies. This table was created by the HEASARC in July 2012 based on an electronic version of Table 6 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
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Search Results
- ID:
- ivo://CDS.VizieR/J/ApJS/170/288
- Title:
- WMAP 3 Year Temperature Analysis
- Short Name:
- J/ApJS/170/288
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present new full-sky temperature maps in five frequency bands from 23 to 94GHz, based on data from the first 3 years of the WMAP sky survey. The new maps are consistent with the first-year maps and are more sensitive. We employ two forms of multifrequency analysis to separate astrophysical foreground signals from the CMB, each of which improves on our first-year analyses. First, we form an improved "Internal Linear Combination" (ILC) map, based solely on WMAP data, by adding a bias-correction step and by quantifying residual uncertainties in the resulting map. Second, we fit and subtract new spatial templates that trace Galactic emission; in particular, we now use low-frequency WMAP data to trace synchrotron emission instead of the 408MHz sky survey. The WMAP point source catalog is updated to include 115 new sources whose detection is made possible by the improved sky map sensitivity. We derive the angular power spectrum of the temperature anisotropy using a hybrid approach that combines a maximum likelihood estimate at low l (large angular scales) with a quadratic cross-power estimate for l>30. The resulting multifrequency spectra are analyzed for residual point source contamination. At 94GHz the unmasked sources contribute 128+/-27^{micron}^K^2^ to l(l+1)C_l_/2{pi} at l=1000. After subtracting this contribution, our best estimate of the CMB power spectrum is derived by averaging cross-power spectra from 153 statistically independent channel pairs. A simple six-parameter {LAMBDA}CDM model continues to fit CMB data and other measures of large-scale structure remarkably well. The new polarization data produce a better measurement of the optical depth to reionization, {tau}=0.089+/-0.03. This new and tighter constraint on {tau} help break a degeneracy with the scalar spectral index, which is now found to be ns=0.960+/-0.016.
- ID:
- ivo://CDS.VizieR/J/MNRAS/400/984
- Title:
- WMAP 3-yr sources at 16 and 33GHz
- Short Name:
- J/MNRAS/400/984
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present follow-up observations of 97 point sources from the Wilkinson Microwave Anisotropy Probe (WMAP) 3-yr data, contained within the New Extragalactic WMAP Point Source catalogue between -4{deg}<=DE<=60{deg}; the sources form a flux-density-limited sample complete to 1.1Jy (~5{sigma}) at 33GHz. Our observations were made at 16GHz using the Arcminute Microkelvin Imager and at 33GHz with the Very Small Array (VSA).
- ID:
- ivo://CDS.VizieR/J/MNRAS/400/995
- Title:
- WMAP 3-yr sources at 16 and 33GHz. II.
- Short Name:
- J/MNRAS/400/995
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using the Arcminute Microkelvin Imager (AMI) at 16GHz and the Very Small Array (VSA) at 33GHz to make follow-up observations of sources in the New Extragalactic WMAP Point Source catalogue, we have investigated the flux density variability in a complete sample of 97 sources over time-scales of a few months to ~1.5yr.
24805. W. M. Keck Observatory
- ID:
- ivo://KeckObs/KeckObs
- Title:
- W. M. Keck Observatory
- Short Name:
- Keck
- Date:
- 04 Apr 2008 16:43:32
- Publisher:
- W. M. Keck Observatory, CARA
- Description:
- The Keck Observatory's instruments are the twin Keck Telescopes, the world's largest optical and infrared telescopes. Each stands eight stories tall and weighs 300 tons, yet operates with nanometer precision. At the heart of each Keck Telescope is a revolutionary primary mirror. Ten meters in diameter, the mirror is composed of 36 hexagonal segments that work in concert as a single piece of reflective glass.
- ID:
- ivo://msc.koa/hires
- Title:
- W. M. Keck Observatory Archive
- Short Name:
- KOA
- Date:
- 11 Jul 2006 18:51:46
- Publisher:
- Michelson Science Center
- Description:
- The W. M. Keck Observatory Archive (KOA) serves level 0 (uncalibrated) observations made with the CCD mosaic upgrade to the High Resolution Echelle Spectrograph (HIRES), commissioned on the Keck Telescope in August 2004. The data are subject to the proprietary policy agreed upon by NASA and the California Association for Research in Astronomy (CARA).
- ID:
- ivo://msc.koa
- Title:
- W. M. Keck Observatory Archive
- Short Name:
- KOA
- Date:
- 11 Jul 2006 14:21:22
- Publisher:
- Michelson Science Center
- Description:
- This resource represents the naming authority for the Michelson Science Center and the W. M. Keck Observatory Archive (KOA)
- ID:
- ivo://KeckObs
- Title:
- W. M. Keck Observatory Authority Name
- Short Name:
- Keck
- Date:
- 04 Apr 2008 16:43:47
- Publisher:
- W. M. Keck Observatory
- Description:
- This naming authority is for identifying resources from the Keck Observatory.
- ID:
- ivo://CDS.VizieR/J/A+A/636/A38
- Title:
- W43-MM1 ALMA ^12^CO(2-1) datacube
- Short Name:
- J/A+A/636/A38
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The accretion history of protostars remains widely mysterious even though it represents one of the best ways to understand the protostellar collapse that leads to the formation of stars. Molecular outflows, which are easier to detect than the direct accretion onto the prostellar embryo, are here used to characterize the protostellar accretion phase in W43-MM1. The W43-MM1 protocluster hosts a sufficient number of protostars to statistically investigate molecular outflows in a single, homogeneous region. We used the CO(2-1) and SiO(5-4) line datacubes, taken as part of an ALMA mosaic with a 2000 AU resolution, to search for protostellar outflows, evaluate the influence that the environment has on these outflows' characteristics and put constraints on outflow variability in W43-MM1. We discovered a rich cluster of 46 outflow lobes, driven by 27 protostars with masses of 1-100M_{sun}_. The complex environment inside which these outflow lobes develop has a definite influence on their length, limiting the validity of using outflow's dynamical timescales as a proxy of the ejection timescale in clouds with high dynamics and varying conditions. We performed a detailed study of Position-Velocity (PV) diagrams of outflows that revealed clear events of episodic ejection. The time variability of W43-MM1 outflows is a general trend and is more generally observed than in nearby, low- to intermediate-mass star-forming regions. The typical timescale found between two ejecta, ~500yr, is consistent with that found in nearby protostars. If ejection episodicity reflects variability in the accretion process, either protostellar accretion is more variable or episodicity is easier to detect in high-mass star-forming regions than in nearby clouds. The timescale found between accretion events could be resulting from instabilities, associated with bursts of inflowing gas arising from the close dynamical environment of highmass star-forming cores.
- ID:
- ivo://CDS.VizieR/J/ApJ/393/149
- Title:
- W49N H2O maser outflow: distance and kinematics
- Short Name:
- J/ApJ/393/149
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Study of the motions of 105 H2O maser features clustered around a newly formed star in W49N yields the kinematics of the gas flow, the distance to the source, and the spatial scale of the Milky Way. We find that the maser outflow is bipolar, with an opening angle of ~60deg and an inclination of ~40deg to the line of sight. The expansion has a constant velocity of ~18 km/s out to a radius of 0.1pc, beyond which the outflow velocity increases to greater than 200 km/s. This increase may be due to interaction with ambient material. A rotation is also present; this rotation is nearly perpendicular to the outflow axis. The rotation may be due to ram pressure from ambient material; rotation of the ring of H II regions described by Welch et al. could produce such nonradial motion. Comparison of Doppler velocities and proper motions yields a distance of 11.4+/-1.2 kpc for the maser cluster. Combining this with a kinematic distance for W49N from Galactic rotation, we obtain a value of R0, the distance to the Galactic center, of 8.1+/-1.1 kpc.
