The UKIRT Infrared Deep Sky Survey Early Data Release

Dye, S.; Warren, S. J.; Hambly, N. C.; Cross, N. J. G.; Hodgkin, S. T.; Irwin, M. J.; Lawrence, Andy; Adamson, A. J.; Almaini, O.; Edge, A. C.; Hirst, Paul; Jameson, R. F.; Lucas, P. W.; Breukelen, C. van; Bryant, Julia J.; Casali, M.; Collins, R. S.; Dalton, Gavin; Davies, Jonathan Ivor; Davis, C. J.; Emerson, J. P.; Evans, D. W.; Foucaud, S.; Gonzales-Solares, E.; Hewett, Paul C.; Kendall, T. R.; Kerr, Tom; Leggett, S. K.; Lodieu, N.; Loveday, Jon; Lewis, Jim; Mann, Robert; McMahon, R. G.; Mortlock, D.; Nakajima, Yasushi; Pinfield, D. J.; Rawlings, Mark G.; Read, Mike; Riello, M.; Sekiguchi, K.; Smith, A. J.; Sutorius, Eckhard; Varricatt, W. P.; Walton, N. A.; Weatherley, S. J.

doi:10.1111/j.1365-2966.2006.10928.x

Cited by 190 publications

(223 citation statements)

References 12 publications

(14 reference statements)

Supporting

Mentioning

218

Contrasting

Order By: Relevance

“…The UKIDSS has a 5σ limiting magnitude of 18.1 mag in the K-band (Dye et al 2006;Lawrence et al 2007), whereas the K-band magnitude limit (10σ) of 2MASS is 14.3 mag (Skrutskie et al 2006). This prompted us to study the effect of sensitivity on cluster detection using the conventional techniques.…”

Section: Revisiting the Cluster Associated With Iras 20286+4105mentioning

confidence: 99%

“…In this work we use K-band (2.20 µm) data from the UKIDSS 8PLUS Galactic Plane Survey (GPS) which has a resolution of ∼ 1 and 5 σ limiting magnitude of K = 18.1 mag (Dye et al 2006). As discussed in Lucas et al (2008), in order to get an estimate of the star count in our field of interest, we filter the sources classified as 'noise' and retain those with mergedClass values of -1 or -2 that denotes a star or probable star.…”

Section: Near-infrared Data From Ukidssmentioning

confidence: 99%

See 1 more Smart Citation

Radio and infrared study of the star-forming region IRAS 20286+4105

Ramachandran

Das

Tej

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

A multi-wavelength investigation of the star forming complex IRAS 20286+4105, located in the Cygnus-X region, is presented here. Near-infrared K-band data is used to revisit the cluster / stellar group identified in previous studies. The radio continuum observations, at 610 and 1280 MHz show the presence of a HII region possibly powered by a star of spectral type B0 -B0.5. The cometary morphology of the ionized region is explained by invoking the bow-shock model where the likely association with a nearby supernova remnant is also explored. A compact radio knot with non-thermal spectral index is detected towards the centre of the cloud. Mid-infrared data from the Spitzer Legacy Survey of the Cygnus-X region show the presence of six Class I YSOs inside the cloud. Thermal dust emission in this complex is modelled using Herschel far-infrared data to generate dust temperature and column density maps. Herschel images also show the presence of two clumps in this region, the masses of which are estimated to be ∼ 175 M and 30 M . The mass-radius relation and the surface density of the clumps do not qualify them as massive star forming sites. An overall picture of a runaway star ionizing the cloud and a triggered population of intermediate-mass, Class I sources located toward the cloud centre emerges from this multiwavelength study. Variation in the dust emissivity spectral index is shown to exist in this region and is seen to have an inverse relation with the dust temperature.

show abstract

Section: Revisiting the Cluster Associated With Iras 20286+4105mentioning

confidence: 99%

Section: Near-infrared Data From Ukidssmentioning

confidence: 99%

Radio and infrared study of the star-forming region IRAS 20286+4105

Ramachandran

Das

Tej

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

Section: D E N T I F I C At I O N O F W D M S B I Na R I E Smentioning

confidence: 99%

“…This exercise resulted in 9593 WDMS binary candidate spectra which were visually inspected. We also inspected their SDSS images for morphological problems and made use of the GALEX ultraviolet (Martin et al 2005;Morrissey et al 2005) and UKIDSS infrared (Dye et al 2006;Hewett et al 2006;Lawrence et al 2007) magnitudes to probe for the presence of excess flux at the blue and red ends of the SDSS spectra, respectively.We found 872 of the 9593 selected spectra to be genuine WDMS binaries and we considered 47 spectra as WDMS binary candidates. In what follows, we flag an object to be a WDMS binary candidate when the spectrum is that of a white dwarf (main-sequence star) displaying some red (blue) flux excess which cannot be confirmed to arise from a companion due to the lack of GALEX (UKIDSS) magnitudes.…”

mentioning

confidence: 99%

The SDSS spectroscopic catalogue of white dwarf-main-sequence binaries: new identifications from DR 9–12

Rebassa‐Mansergas

Ren

Parsons

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We present an updated version of the spectroscopic catalogue of white dwarf-main-sequence (WDMS) binaries from the Sloan Digital Sky Survey (SDSS). We identify 938 WDMS binaries within the data releases (DR) 9-12 of SDSS plus 40 objects from DR 1-8 that we missed in our previous works, 646 of which are new. The total number of spectroscopic SDSS WDMS binaries increases to 3294. This is by far the largest and most homogeneous sample of compact binaries currently available. We use a decomposition/fitting routine to derive the stellar parameters of all systems identified here (white dwarf effective temperatures, surface gravities and masses, and secondary star spectral types). The analysis of the corresponding stellar parameter distributions shows that the SDSS WDMS binary population is seriously affected by selection effects. We also measure the Na I λλ 8183.27, 8194.81 absorption doublet and H α emission radial velocities (RV) from all SDSS WDMS binary spectra identified in this work. 98 objects are found to display RV variations, 62 of which are new. The RV data are sufficient enough to estimate the orbital periods of three close binaries.Key words: binaries: close -binaries: spectroscopic -stars: low-mass -white dwarfs. I N T RO D U C T I O NA large fraction of main-sequence stars are found in binary systems (Duquennoy & Mayor 1991;Raghavan et al. 2010;Yuan et al. 2015b). It is expected that ∼25 per cent of all main-sequence binaries are close enough to begin mass transfer interactions when the more massive star becomes a red giant or an asymptotic giant star (Willems & Kolb 2004). This has been observationally verified e.g. by Farihi, Hoard & Wachter (2010) and by Nebot . Because the mass transfer rate generally exceeds the Eddington limit, the secondary star is not able to accrete the transferred material and the system evolves through a common envelope phase. That is, the core of the giant and the main-sequence companion orbit within a common envelope formed by the outer layers of the giant star. Drag forces between the two stars and the envelope lead to the shrinkage of the orbit and therefore to the release E-mail: alberto.rebassa@upc.edu of orbital energy. The orbital energy is deposited into the envelope and is eventually used to eject it (Webbink 2008). The outcome of common envelope evolution is hence a close binary formed by the core of the giant star (which later becomes a white dwarf) and a main-sequence companion, i.e. a close white dwarf-main-sequence (WDMS) binary. These are commonly referred to as post-common envelope binaries (PCEBs). The remaining ∼75 per cent of mainsequence binaries are wide enough to avoid mass transfer interactions. In these cases the more massive stars evolve like single stars until they eventually become white dwarfs. The orbital separations of such WDMS binaries are similar to those of the main-sequence binaries from which they descend.During the last years we have mined the Sloan Digital Sky Survey (SDSS; York et al. 2000) spectroscopic data base to build up th...

show abstract

“…Raw photometric catalogues were calibrated on to the system defined by the 2MASS PSC, by applying the color terms between the WFCAM and 2MASS systems (Dye et al 2006). The photometric zero-points were then calculated by comparing our transformed magnitudes with the 2MASS magnitudes for stars in common with the PSC.…”

Section: Observations and Data Reductionmentioning

confidence: 99%