A Far-Ultraviolet Survey of M80: X-Ray Source Counterparts, Strange Blue Stragglers, and the Recovery of Nova T Sco

Dieball, A.; Long, Knox S.; Knigge, Christian; Thomson, Grace S.; Zurek, David

doi:10.1088/0004-637x/710/1/332

Cited by 41 publications

(48 citation statements)

References 51 publications

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“…This is to be expected since it has a U mean magnitude of 19.5 mag. The star V33 was discovered by Dieball et al (2010) in an ultraviolet survey using the Hubble Space Telescope. They reported a UV magnitude for this target of about 19.8 mag.…”

Section: Known Variablesmentioning

confidence: 99%

“…Coloured points follow the convention adopted in Table 2 to identify the types of variables found in the field of this globular cluster. Dieball et al (2010) in their ultraviolet survey assigned the label CX01 to an X-ray source that was found to be associated with the position of the Nova at the coordinates RA(J2000) = 16:17:02.817 and Dec(J2000) = −22:58:33.92. These coordinates match with the position of the outburst found in this work and details are given in Table 7.…”

Section: V34: This Is the Nova Discovered By Arthur Von Auwers At Koementioning

confidence: 99%

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Exploring the crowded central region of ten Galactic globular clusters using EMCCDs

Jaimes¹,

Bramich²,

Skottfelt³

et al. 2016

A&A

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Aims. We aim to obtain time-series photometry of the very crowded central regions of Galactic globular clusters; to obtain better angular resolution than has been previously achieved with conventional CCDs on ground-based telescopes; and to complete, or improve, the census of the variable star population in those stellar systems. Methods. Images were taken using the Danish 1.54-m Telescope at the ESO observatory at La Silla in Chile. The telescope was equipped with an electron-multiplying CCD, and the short-exposure-time images obtained (ten images per second) were stacked using the shift-and-add technique to produce the normal-exposure-time images (minutes). Photometry was performed via difference image analysis. Automatic detection of variable stars in the field was attempted. Results. The light curves of 12 541 stars in the cores of ten globular clusters were statistically analysed to automatically extract the variable stars. We obtained light curves for 31 previously known variable stars (3 long-period irregular, 2 semi-regular, 20 RR Lyrae, 1 SX Phoenicis, 3 cataclysmic variables, 1 W Ursae Majoris-type and 1 unclassified) and we discovered 30 new variables (16 long-period irregular, 7 semi-regular, 4 RR Lyrae, 1 SX Phoenicis and 2 unclassified). Fluxes and photometric measurements for these stars are available in electronic form through the Strasbourg astronomical Data Center.

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Section: Known Variablesmentioning

confidence: 99%

Section: V34: This Is the Nova Discovered By Arthur Von Auwers At Koementioning

confidence: 99%

Exploring the crowded central region of ten Galactic globular clusters using EMCCDs

Jaimes¹,

Bramich²,

Skottfelt³

et al. 2016

A&A

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show abstract

“…Deep ACS observations of NGC 6397 [411] have identified a substantial population of approximately 150 white dwarfs [453]. Dieball et al [107] have found approximately 30 white dwarfs and about 60 probably cataclysmic variables and white dwarf binaries in M80. In general, however, these searches uncover single white dwarfs.…”

Section: Observationsmentioning

confidence: 99%

Relativistic Binaries in Globular Clusters

Benacquista¹,

Downing

2013

Living Rev. Relativ.

198

129

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Galactic globular clusters are old, dense star systems typically containing 104–106 stars. As an old population of stars, globular clusters contain many collapsed and degenerate objects. As a dense population of stars, globular clusters are the scene of many interesting close dynamical interactions between stars. These dynamical interactions can alter the evolution of individual stars and can produce tight binary systems containing one or two compact objects. In this review, we discuss theoretical models of globular cluster evolution and binary evolution, techniques for simulating this evolution that leads to relativistic binaries, and current and possible future observational evidence for this population. Our discussion of globular cluster evolution will focus on the processes that boost the production of tight binary systems and the subsequent interaction of these binaries that can alter the properties of both bodies and can lead to exotic objects. Direct N-body integrations and Fokker-Planck simulations of the evolution of globular clusters that incorporate tidal interactions and lead to predictions of relativistic binary populations are also discussed. We discuss the current observational evidence for cataclysmic variables, millisecond pulsars, and low-mass X-ray binaries as well as possible future detection of relativistic binaries with gravitational radiation.

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“…more massive stars travel towards the cluster centre, but less massive stars, like the HB stars which typically have masses of ≈ 0.5M ⊙ , are pushed out of the dense cluster centre (see e.g. Dieball et al 2010, who derived an average mass of ≈ 0.6M ⊙ for the HB population in M 80).…”

Section: Horizontal Branch Starsmentioning

confidence: 99%

Far-ultraviolet observation of the globular cluster NGC 6397

Dieball

Rasekh

Knigge

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present an observational far-UV (FUV) and near-UV (NUV) study of the core region of the globular cluster NGC 6397. The observations were obtained with the Space Telescope Imaging Spectrograph (STIS, FUV), and the Wide Field Camera 3 (WFC3, NUV) on board the Hubble Space Telescope. Here, we focus on the UV bright stellar populations such as blue stragglers (BSs), white dwarfs (WDs) and cataclysmic variables (CVs). We present the first FUV − NUV color-magnitude diagram (CMD) for this cluster. To support our classification of the stellar populations, we compare our FUV − NUV CMD with optical data from the ACS Survey of Galactic Globular Clusters. The FUV − NUV CMD indicates 16 sources located in the WD area, and ten BSs within the 25 ′′ × 25 ′′ of the STIS FUV data. Eighteen Chandra X-ray sources are located within the FUV field of view. Thirteen of those have a NUV counterpart, of which nine sources also have a FUV counterpart. Out of those, five sources are previously suggested CVs, and indeed all five are located in the WD/CV region in our FUV − NUV CMD. Another CV only has a FUV but no NUV counterpart. We also detect a NUV (but no FUV) counterpart to the MSP located in the core of this cluster. The NUV lightcurves of the CVs and MSP show flickering behaviour typical of CVs. We found that the BSs and CVs are the most centrally concentrated population. This might be an effect of mass segregation or indicate the preferred birth place of BSs and CVs via dynamical interactions in the dense core region of GCs. HB stars are the least centrally concentrated population and absent in the innermost area of the core.

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A Far-Ultraviolet Survey of M80: X-Ray Source Counterparts, Strange Blue Stragglers, and the Recovery of Nova T Sco

Cited by 41 publications

References 51 publications

Exploring the crowded central region of ten Galactic globular clusters using EMCCDs

Exploring the crowded central region of ten Galactic globular clusters using EMCCDs

Relativistic Binaries in Globular Clusters

Far-ultraviolet observation of the globular cluster NGC 6397

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