The UKIDSS Galactic Plane Survey

Lucas, P. W.; Hoare, M. G.; Longmore, A. J.; Schröder, Anja; Davis, C. J.; Adamson, A. J.; Bandyopadhyay, Reba M.; Grijs, Richard de; Smith, Michael D.; Gosling, Amanda; Mitchison, Sharon; Gáspár, András; Coe, M. J.; Tamura, Motohide; Parker, Quentin A.; Irwin, M. J.; Hambly, N. C.; Bryant, Julia J.; Collins, R. S.; Cross, N. J. G.; Evans, D. W.; González-Solares, E.; Hodgkin, S. T.; Lewis, Jim; Read, Mike; Riello, M.; Sutorius, Eckhard; Lawrence, Andy; Drew, J. E.; Dye, S.; Thompson, M. A.

doi:10.1111/j.1365-2966.2008.13924.x

Cited by 491 publications

(492 citation statements)

References 65 publications

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“…The observations of the XMMJ1747 source field were also taken during the UKIDSS Galactic plane survey (Lucas et al 2008) on July 18, 2006 in J, H and K bands. Both stars are visible in the H and K bands, see Figure 1, for the UKIRT K band observations.…”

Section: Xmmu J1747161-281048mentioning

confidence: 99%

“…To calibrate the observations, we used the archival 3.5-meter United Kingdom Infra-red Tele-scope (UKIRT) observations of the source field in J, H and K bands which were obtained as a part of the UKIDSS Galactic plane survey (Lucas et al 2008). These observations were taken on July 18, 2006 for XMM1747 and July 23, 2006 for SAX1806 using the wide field infrared camera (WFCAM) composed of four Rockwell Hawaii-II 2048 × 2048 18 micron pixel array detectors, with a pixel scale of 0.…”

Section: Data Reduction and Analysismentioning

confidence: 99%

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A search for near-infrared counterparts of two faint neutron star X-ray transients: XMMU J174716.1−281048 and SAX J1806.5−2215

Kaur

Wijnands

Kamble

et al. 2016

Mon. Not. R. Astron. Soc.

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We present our near-infrared (NIR) imaging observations of two neutron star low mass X-ray binaries XMMU J174716.1-281048 and SAX J1806.5-2215 obtained using the PANIC instrument on the 6.5-meter Magellan telescope and the WHIRC instrument on the 3.5-meter WIYN telescope respectively. Both sources are members of the class of faint to very-faint X-ray binaries and undergo very long X-ray outburst, hence classified as 'quasi persistent X-ray binaries'. While XMMU J174716.1-281048 was active for almost 12 years between 2003 and 2015, SAX J1806.5-2215 has been active for more than 5 years now since 2011. From our observations, we identify two NIR stars consistent with the Chandra X-ray error circle of XMMU J174716.1-281048. The comparison of our observations with the UKIRT Galactic plane observations taken during the same outburst, color-color diagram analysis and spectral energy distribution suggest that both stars are probably a part of the field population and are likely high mass stars. Hence possibly neither of the two stars is a true NIR counterpart. For the faint X-ray binary SAX J1806.5-2215 during its current outburst, we detected a NIR star in our K band WIYN observations consistent with its Chandra error circle. The identified NIR star was not detected during the UKIRT observations taken during its quiescent state. The comparison of two observations suggest that there was an increase in flux by at least one magnitude of the detected star during our observations, hence suggests the detection of the likely counterpart of SAX J1806.5-2215.

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Section: Xmmu J1747161-281048mentioning

confidence: 99%

Section: Data Reduction and Analysismentioning

confidence: 99%

A search for near-infrared counterparts of two faint neutron star X-ray transients: XMMU J174716.1−281048 and SAX J1806.5−2215

Kaur

Wijnands

Kamble

et al. 2016

Mon. Not. R. Astron. Soc.

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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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“…By comparison to optical observations, infrared photometry suffers an order of magnitude less dust obscuration (e.g., A [4.5µm] ∼ 0.05A V , Flaherty et al 2007). Forthcoming results from the VVV/UKIDSS near -infrared surveys (Lucas et al 2008;Minniti et al 2010) are thus pertinent for detecting YSOs and their host clusters, and the observations will extend ∼ 4 m fainter than 2MASS for Galactic disk stars. The VVV survey shall establish precise multi- Minniti et al 2010;Catelan et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Discovering protostars and their host clusters via WISE

Majaess¹

2012

Astrophys Space Sci

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A hybrid JHK s − W 1 W 2 W 3 W 4 high-spectral index (α) selection scheme was employed to identify (sub)clusters of class I/f candidate protostars (YSOs) in WISE observations (the Wide-Field Infrared Survey Explorer). n > 10 4 candidate YSOs were detected owing to WISE's advantageous all-sky spatial coverage, and a subsample (n ∼ 200) of their heavily-obscured host (sub)clusters were correlated with the Avedisova (2002) and Dias et al. (2002) catalogs of star-forming regions. Forthcoming observations from the VVV/UKIDSS surveys shall facilitate the detection of additional protostars and bolster efforts to delineate the Galactic plane, since the campaigns aim to secure deep JHK s photometry for a pertinent fraction of the WISE targets lacking 2MASS detections, and to provide improved data for YSOs near the limits of the 2MASS survey.

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The UKIDSS Galactic Plane Survey

Cited by 491 publications

References 65 publications

A search for near-infrared counterparts of two faint neutron star X-ray transients: XMMU J174716.1−281048 and SAX J1806.5−2215

A search for near-infrared counterparts of two faint neutron star X-ray transients: XMMU J174716.1−281048 and SAX J1806.5−2215

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

Discovering protostars and their host clusters via WISE

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