The<i>Spitzer</i>/GLIMPSE Surveys: A New View of the Milky Way

Churchwell, E.; Babler, B.; Meade, M. R.; Whitney, B. A.; Benjamin, Robert A.; Indebetouw, R.; Cyganowski, C. J.; Robitaille, Thomas; Povich, Matthew S.; Watson, C.; Bracker, S.

doi:10.1086/597811

Cited by 959 publications

(958 citation statements)

References 82 publications

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“…A1, page 10 of 22 iv) the MaxBCG galaxy clusters catalogue from SDSS (Koester et al 2007); v) the 2XMMi/SDSS DR7 cross-correlation (Pineau et al 2011); vi) the 3rd release of the RAVE catalogue (Siebert et al 2011); vii) the IPHAS Hα emission line source catalogue (Witham et al 2008); viii) the WISE All-Sky data Release (Cutri & et al 2012); ix) the AKARI mid-IR all-sky survey (Ishihara et al 2010) and version 1.0 of the all-sky survey bright source catalogue (Yamamura et al 2010); x) the Spitzer IRAC survey of the galactic center (Ramírez et al 2008); xi) the GLIMPSE Source Catalogue (I + II + 3D Churchwell et al 2009); xii) the IRAC-24 micron optical source catalogue (Surace et al 2004); and xiii) the Planck Early Release Compact Source Catalogue (Planck Collaboration VII 2011). Table 4 lists, for a selection of archival catalogues, the number of EPIC detections having at least one catalogue entry in the 99.73% (3 Gaussian σ) confidence region.…”

Section: External Catalogue Cross-correlationmentioning

confidence: 99%

TheXMM-Newtonserendipitous survey

Rosen

Webb

Watson

et al. 2016

A&A

318

150

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Context. Thanks to the large collecting area (3 × ∼1500 cm 2 at 1.5 keV) and wide field of view (30 across in full field mode) of the X-ray cameras on board the European Space Agency X-ray observatory XMM-Newton, each individual pointing can result in the detection of up to several hundred X-ray sources, most of which are newly discovered objects. Since XMM-Newton has now been in orbit for more than 15 yr, hundreds of thousands of sources have been detected. Aims. Recently, many improvements in the XMM-Newton data reduction algorithms have been made. These include enhanced source characterisation and reduced spurious source detections, refined astrometric precision of sources, greater net sensitivity for source detection, and the extraction of spectra and time series for fainter sources, both with better signal-to-noise. Thanks to these enhancements, the quality of the catalogue products has been much improved over earlier catalogues. Furthermore, almost 50% more observations are in the public domain compared to 2XMMi-DR3, allowing the XMM-Newton Survey Science Centre to produce a much larger and better quality X-ray source catalogue. Methods. The XMM-Newton Survey Science Centre has developed a pipeline to reduce the XMM-Newton data automatically. Using the latest version of this pipeline, along with better calibration, a new version of the catalogue has been produced, using XMM-Newton X-ray observations made public on or before 2013 December 31. Manual screening of all of the X-ray detections ensures the highest data quality. This catalogue is known as 3XMM. Results. In the latest release of the 3XMM catalogue, 3XMM-DR5, there are 565 962 X-ray detections comprising 396 910 unique X-ray sources. Spectra and lightcurves are provided for the 133 000 brightest sources. For all detections, the positions on the sky, a measure of the quality of the detection, and an evaluation of the X-ray variability is provided, along with the fluxes and count rates in 7 X-ray energy bands, the total 0.2-12 keV band counts, and four hardness ratios. With the aim of identifying the detections, a cross correlation with 228 catalogues of sources detected in all wavebands is also provided for each X-ray detection. Conclusions. 3XMM-DR5 is the largest X-ray source catalogue ever produced. Thanks to the large array of data products associated with each detection and each source, it is an excellent resource for finding new and extreme objects.Key words. catalogs -astronomical databases: miscellaneous -surveys -X-rays: general Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA.The catalogue is available at http://cdsarc.u-strasbg.fr/ viz-bin/VizieR?-meta.foot&-source=IX/46

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Section: External Catalogue Cross-correlationmentioning

confidence: 99%

TheXMM-Newtonserendipitous survey

Rosen

Webb

Watson

et al. 2016

A&A

318

150

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“…This observation was designed to be combined with near-and mid-IR photometry from the Spitzer Space Telescope Galactic Legacy IR Mid-Plane Survey Extraordinaire (GLIMPSE; Benjamin et al 2003;Churchwell et al 2009) and MIPSGAL Galactic plane survey (Carey et al 2009), 2MASS, and the UKIDSS Galactic Plane Survey (Lawrence et al 2007;Lucas et al 2008). In Section 2 we present the various data sets used for our study.…”

Section: Introductionmentioning

confidence: 99%

RAPID CIRCUMSTELLAR DISK EVOLUTION AND AN ACCELERATING STAR FORMATION RATE IN THE INFRARED DARK CLOUD M17 SWex

Povich

Townsley

Robitaille

et al. 2016

ApJ

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We present a catalog of 840 X-ray sources and first results from a 100 ks Chandra X-ray Observatory imaging study of the filamentary infrared (IR) dark cloud G014.225-00.506, which forms the central regions of a larger cloud complex known as the M17 southwest extension (M17 SWex). In addition to the rich population of protostars and young stellar objects with dusty circumstellar disks revealed by archival data from the Spitzer Space Telescope, we discover a population of X-ray-emitting, intermediate-mass pre-main-sequence stars that lack IR excess emission from circumstellar disks. We model the IR spectral energy distributions of this source population to measure its mass function and place new constraints on the destruction timescales for the inner dust disk for 2-8 M ☉ stars. We also place a lower limit on the star formation rate (SFR) and find that it is quite high (  M 0.007 M ☉ yr −1 ), equivalent to several Orion Nebula Clusters in G14.225-0.506 alone, and likely accelerating. The cloud complex has not produced a population of massive, O-type stars commensurate with its SFR. This absence of very massive (20 M ☉ ) stars suggests that either (1) M17 SWex is an example of a distributed mode of star formation that will produce a large OB association dominated by intermediate-mass stars but relatively few massive clusters, or (2) the massive cores are still in the process of accreting sufficient mass to form massive clusters hosting O stars.

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“…To visualize and examine the environment of the VYSOs, we composed color images using the Spitzer MIPSGAL (Carey et al 2009) and GLIMPSE (Churchwell et al 2009) cutouts and overlaid contours of 850μm emission from the ATLAS-GAL data. In Figure 1 (left panel) we display such an overlay for the source VVVv374.…”

Section: High-amplitude Variable Stars Within Atlasgal Clumpsmentioning

confidence: 99%

Highly Variable Young Massive Stars in Atlasgal Clumps

Kumar

Peña

Lucas

2016

ApJ

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High-amplitude variability in young stellar objects (YSOs) is usually associated with episodic accretion events. It has not been observed so far in massive YSOs. Here, the high-amplitude variable star sample of Contreras Peña et al. has been used to search for highly variable (ΔK 1 mag) sources coinciding with dense clumps mapped using the 850μm continuum emission by the ATLASGAL survey. A total of 18 variable sources are centered on the submillimeter clump peaks and coincide (<1″) with a 24μm point or compact (<10″) source. Of these 18 sources, 13 can be fit by YSO models. The 13 variable YSOs (VYSOs) have luminosities of ∼10 3 L e , an average mass of 8M e , and a range of ages up to 10 6 yr. A total of 11 of these 13 VYSOs are located in the midst of infrared dark clouds. Nine of the 13 sources have ΔK>2 mag, significantly higher compared to the mean variability of the entire VVV sample. The light curves of these objects sampled between 2010 and 2015 display rising, declining, or quasi-periodic behavior but no clear periodicity. Light-curve analysis using the Plavchan method shows that the most prominent phased signals have periods of a few hundred days. The nature and timescale of variations found in 6.7 Ghz methanol maser emission in massive stars are similar to that of the VYSO light curves. We argue that the origin of the observed variability is episodic accretion. We suggest that the timescale of a few hundred days may represent the frequency at which a spiraling disk feeds dense gas to the young massive star.

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TheSpitzer/GLIMPSE Surveys: A New View of the Milky Way

Cited by 959 publications

References 82 publications

TheXMM-Newtonserendipitous survey

TheXMM-Newtonserendipitous survey

RAPID CIRCUMSTELLAR DISK EVOLUTION AND AN ACCELERATING STAR FORMATION RATE IN THE INFRARED DARK CLOUD M17 SWex

Highly Variable Young Massive Stars in Atlasgal Clumps

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