The ROTSE‐III Robotic Telescope System

Akerlof, C.; Kehoe, R.; McKay, Timothy A.; Rykoff, E. S.; Smith, D. A.; Casperson, D.; McGowan, K.; Vestrand, W. T.; Woźniak, P. R.; Wren, J.; Ashley, M. C. B.; Phillips, Michael A.; Marshall, Stuart; Schier, Jan

doi:10.1086/345490

Cited by 186 publications

(168 citation statements)

References 18 publications

Supporting

Mentioning

167

Contrasting

Unclassified

Order By: Relevance

“…The TSS employed the 0.45-m ROTSE-IIIb telescope at the McDonald observatory in Texas, and the data presented here are supplemented by its twin, the ROTSE-IIId telescope, which is located at the Turkish National Observatory at Bakirlitepe, Turkey. The ROTSE-III system is described in Akerlof et al (2003). The 1.…”

Section: Optical Observationsmentioning

confidence: 99%

The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

Henze

Pietsch

Haberl

et al. 2009

A&A

View full text Add to dashboard Cite

Context. Classical novae (CNe) have been found to represent the major class of supersoft X-ray sources (SSSs) in our neighbour galaxy M 31. Aims. We determine the properties and evolution of the two first SSSs ever discovered in the M 31 globular cluster (GC) system. Methods. We have used XMM-Newton, Chandra and Swift observations of the centre region of M 31 to discover both SSSs and to determine their X-ray light curves and spectra. We performed detailed analysis of XMM-Newton EPIC PN spectra of the source in Bol 111 (SS1) using blackbody and NLTE white dwarf (WD) atmosphere models. For the SSS in Bol 194 (SS2) we used optical monitoring data to search for an optical counterpart. Results. Both GC X-ray sources were classified as SSS. We identify SS1 with the CN M31N 2007-06b recently discovered in the M 31 GC Bol 111. For SS2 we did not find evidence for a recent nova outburst and can only provide useful constraints on the time of the outburst of a hypothetical nova. Conclusions. The only known CN in a M 31 GC can be identified with the first SSS found in a M 31 GC. We discuss the impact of our observations on the nova rate for the M 31 GC system.

show abstract

Section: Optical Observationsmentioning

confidence: 99%

The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

Henze

Pietsch

Haberl

et al. 2009

A&A

View full text Add to dashboard Cite

show abstract

“…A recent example is SN 2010kd, discovered by the ROTSE robotic telescope [69] at the University of Texas. Figure 10 shows the light curve of this supernova obtained by ROTSE and several models of the light curve [68,70,71].…”

Section: (B) Core-collapse Supernovaementioning

confidence: 99%

Astrophysical explosions: from solar flares to cosmic gamma-ray bursts

Wheeler

2012

Phil. Trans. R. Soc. A.

View full text Add to dashboard Cite

Astrophysical explosions result from the release of magnetic, gravitational or thermonuclear energy on dynamical time scales, typically the sound-crossing time for the system. These explosions include solar and stellar flares, eruptive phenomena in accretion discs, thermonuclear combustion on the surfaces of white dwarfs and neutron stars, violent magnetic reconnection in neutron stars, thermonuclear and gravitational collapse supernovae and cosmic gamma-ray bursts, each representing a different type and amount of energy release. This paper summarizes the properties of these explosions and describes new research on thermonuclear explosions and explosions in extended circumstellar media. Parallels are drawn between studies of terrestrial and astrophysical explosions, especially the physics of the transition from deflagration-to-detonation.

show abstract

“…QE (Quantum Efficiency) of the CCD peaks at 550 nm. The telescope and CCD were described in Akerlof et al (2003). The CCD observations have been carried out in three different exposure times: 5 (∼ 54%), 20 and 60 seconds.…”

Section: Rotse-iiidobservations and Structure Of The Datamentioning

confidence: 99%

“…The pointing accuracy (or error) of the ROTSE-IIIdtelescope is given as approximately 1 ′ (Akerlof et al, 2003).…”

Section: Stage-b: Astrometry Of Field Starsmentioning

confidence: 99%

See 1 more Smart Citation

A pipeline for the ROTSE–IIId archival data

et al. 2012

View full text Add to dashboard Cite

We have constructed a new, fast, robust and reliable pipeline to detect variable stars from the ROTSE-IIId archival data. Turkish share of ROTSE-III archive contains approximately one million objects from a large field of view (1.85 • ) and it considerably covers a large portion of northern sky (δ > −25 • ). The unfiltered ROTSE-III magnitude of the objects ranges from 7.7 to 16.9. The main stages of the new pipeline are as follows: Source extraction, astrometry of the objects, light curve generation and inhomogeneous ensemble photometry. A high performance computing (HPC) algorithm has also been implemented into the pipeline where we had a good performance even on a personal computer. Running the algorithms of the pipeline on a cluster decreases analysis time significantly from weeks to hours. The pipeline is especially tested against long period variable stars with periods of a few hundred days (e.g Mira and SR) and variables having periods starting from a few days to a few hundred days were detected.

show abstract

The ROTSE‐III Robotic Telescope System

Cited by 186 publications

References 18 publications

The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

Astrophysical explosions: from solar flares to cosmic gamma-ray bursts

A pipeline for the ROTSE–IIId archival data

Contact Info

Product

Resources

About