Erupting Dwarf Novae in the Large Magellanic Cloud

Shara, Michael M.; Hinkley, Sasha; Zurek, David

doi:10.1086/379307

Cited by 4 publications

(5 citation statements)

References 21 publications

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“…Since PopI dwarf novae are located nearby the Sun, they have been found and well studied (Coppejans et al 2016;Otulakowska-Hypka et al 2016). In the case of PopII, although there have been attempts to find distant dwarf novae (possible PopII) in halo or thick disk (Hawkins & Veron 1987;Howell & Szkody 1990;Shara et al 2003), few candidates have been found because they reside at large distance from the Sun. Notably, no distance (>5 kpc from the Sun) PopII dwarf nova has been observed with light curves other than the nearby (250 pc) source SDSSJ1507+52 (Uthas et al 2011).…”

Section: Halo or Thick Disk Dwarf Novaementioning

confidence: 99%

KSP-OT-201611a: A Distant Population II Dwarf Nova Candidate Discovered by the KMTNet Supernova Program

Lee

Moon

Kim

et al. 2019

ApJ

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We present a multi-color, high-cadence photometric study of a distant dwarf nova KSP-OT-201611a discovered by the Korea Microlensing Telescope Network Supernova Program. From October 2016 to May 2017, two outbursts, which comprises a super/long outburst followed by a normal/short outburst separated by ∼91 days, were detected in the BV I bands. The shapes and amplitudes of the outbursts reveal the nature of KSP-OT-201611a to be an SU UMa-or U Gem-type dwarf nova. Color variations of periodic humps in the super/long outbutst possibly indicate that KSP-OT-201611a is an SU UMatype dwarf nova. The super and normal outbursts show distinctively different color evolutions during the outbursts due most likely to the difference of time when the cooling wave is formed in the accretion disk. The outburst peak magnitudes and the orbital period of the dwarf nova indicate that it is at a large Galactocentric distance (∼13.8 kpc) and height (∼1.7 kpc) from the Galactic plane. KSP-OT-201611a, therefore, may provide a rare opportunity to study the accretion disk process of Population II dwarf novae.

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Section: Halo or Thick Disk Dwarf Novaementioning

confidence: 99%

KSP-OT-201611a: A Distant Population II Dwarf Nova Candidate Discovered by the KMTNet Supernova Program

Lee

Moon

Kim

et al. 2019

ApJ

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“…All images were de-biased and flat-fielded using SOI Reduction Scripts * . With the help of the Difference Image Analysis Package (DIAPL) † , which is a modified version of DIA written by Woźniak (2000), we subtracted R-band images from images taken in the Hα filter (or vice versa if an Hα image had a lower seeing). We used the ESO Online Digital Sky Survey (DSS) to set equatorial coordinates in each image.…”

Section: Observations and Data Reductionsmentioning

confidence: 99%

“…It has one of the largest and most concentrated population of blue stragglers (over 300) ever observed in a globular cluster (Ferraro et al 1999). NGC 6093 is known to harbor two dwarf novae (DN1 and DN2, Shara et al 2005) and a classical nova (nova 1860 T Sco, Shara and Drissen 1995). The cluster's X-ray population is rich.…”

Section: Ngc 6093 (M80)mentioning

confidence: 99%

H-alpha Imaging of X-ray Sources in Selected Globular Clusters with the SOAR Telescope

Pietrukowicz

2009

Preprint

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We present results of a search for objects with Hα excess, such as cataclysmic variables (CVs) and chromospherically active binaries (ABs), as counterparts to X-ray sources detected with Chandra satellite observatory in six Galactic globular clusters (GCs): M4, M28, M30, M71, M80, NGC 6752. Binary systems play a critical role in the evolution of GCs, serving as an internal energy source countering the tendency of GC cores to collapse. Theoretical studies predict dozens of CVs in the cores of some GCs (e.g., 130 for M28, 40 for M30). A number of such binaries is also expected outside the core radius. However, few CVs are known so far in GCs. Using subtraction technique applied to images taken with the 4.1-m SOAR telescope we have found 27 objects with Hα excess in the field of the observed clusters, of which nine are likely associated with the clusters. Four are candidate CVs, four candidate ABs, one could be either a CV or an AB. One Hα object seems to be a background galaxy, while other 17 detected objects are probably foreground or background stars.

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“…The second nova ever in a globular cluster; and Shara et al (2004) had to go all the way to M31 to see it (well, not literally). The first was T Sco in 1860, reported by N. R. Pogson of the magnitude system and G. F. Auwers, who owned the best-available angular diameter for the Sun at about the same time (he must have worked very long days).…”

Section: Globular Clusters (Of Stars)mentioning

confidence: 99%

“…QSO sight line with four damped Lya absorption systems (Prochaska et al 2003). dwarf nova outside the Milky Way, in the Large Magellanic Cloud (Shara et al 2003). mass-accreting T Tauri star outside the Milky Way.…”

Section: Firstsmentioning

confidence: 99%