THE ALLEN TELESCOPE ARRAY Pi GHz SKY SURVEY. I. SURVEY DESCRIPTION AND STATIC CATALOG RESULTS FOR THE BOÖTES FIELD

Bower, Geoffrey C.; Croft, Steve; Keating, Garrett K.; Whysong, D.; Ackermann, R. F.; Atkinson, Shannon; Backer, D. C.; Backus, P. R.; Barott, Billy; Bauermeister, Amber; Blitz, Leo; Bock, Douglas C.-J.; Bradford, Tucker; Cheng, C.; Cork, C.; Davis, Mike; DeBoer, D.; Dexter, Matt; Dreher, J. W.; Engargiola, G.; Fields, Ed; Fleming, M.; Forster, R.; Gutierrez-Kraybill, Colby; Harp, G. R.; Heiles, Carl; Helfer, Tamara T.; Hull, Chat; Jordan, Jane; Jørgensen, Stine; Kilsdonk, Tom; Law, Casey J.; Leeuwen, J. van; Lugten, J. B.; MacMahon, Dave; McMahon, Peter L.; Milgrome, O.; Pierson, Tom; Randall, Kevin J.; Ross, John E.; Shostak, Seth; Siemion, Andrew; Smolek, Ken; Tarter, Jill; Thornton, D.; Urry, Lynn; Vitouchkine, Artyom; Wadefalk, Niklas; Weinreb, S.; Welch, Jack; Werthimer, Dan; Williams, Peter K. G.; Wright, M. C. H.

doi:10.1088/0004-637x/725/2/1792

Cited by 30 publications

(33 citation statements)

References 54 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Early blind searches have already uncovered multiple variable and transient radio sources (Hyman et al 2005;Lorimer et al 2007;Bower et al 2007Bower et al , 2010Burke-Spolaor & Bailes 2010). However, a majority of the observations were performed at gigahertz (cm to mm wavelength) frequencies, leaving the sub-gigahertz (meter wavelength) sky vastly unexplored.…”

Section: Introductionmentioning

confidence: 99%

Discovery of a Meter-Wavelength Radio Transient in the Swire Deep Field: 1046+59

Jaeger

Hyman

Kassim

et al. 2012

The Astronomical Journal

View full text Add to dashboard Cite

We report the results of a low frequency radio variability and slow transient search using archival observations from the Very Long Array. We selected six 325 MHz radio observations from the spring of 2006, each centered on the Spitzer-Space-Telescope Wide-area Infrared Extragalactic Survey (SWIRE) Deep Field: 1046+59. Observations were spaced between one day to three months, with a typical single-epoch peak flux sensitivity below 0.2 mJy beam −1 near the field pointing center. We describe the observation parameters, data post-processing, and search methodology used to identify variable and transient emission. Our search revealed multiple variable sources and the presence of one, day-scale transient event with no apparent astronomical counterpart. This detection implies a transient rate of 1 ± 1 event per 6.5 deg 2 per 72 observing hours in the direction of 1046+59 and an isotropic transient surface density Σ = 0.12 deg −2 at 95% confidence for sources with average peak flux density higher than 2.1 mJy over 12 hr.

show abstract

Section: Introductionmentioning

confidence: 99%

Discovery of a Meter-Wavelength Radio Transient in the Swire Deep Field: 1046+59

Jaeger

Hyman

Kassim

et al. 2012

The Astronomical Journal

View full text Add to dashboard Cite

show abstract

“…As this is the first transient survey in the millimeter band, comparison of these results to previous surveys (e.g., Levinson et al 2002;Gal-Yam et al 2006;Bower et al 2010;Bell et al 2011;Bower & Saul 2011;Croft et al 2011) is a complex and model-dependent task. The highest frequency of these (Bower et al 2010) was conducted at 5 GHz, a factor of 30 below our primary observing band, and correspondingly was focused on somewhat different sources.…”

Section: Population Constraintsmentioning

confidence: 99%

“…The highest frequency of these (Bower et al 2010) was conducted at 5 GHz, a factor of 30 below our primary observing band, and correspondingly was focused on somewhat different sources. The most similar previous results in terms of science goals, in Levinson et al (2002) and GalYam et al (2006), focus on GRB afterglows, though at lower frequencies (1.4 GHz).…”

Section: Population Constraintsmentioning

confidence: 99%

MILLIMETER TRANSIENT POINT SOURCES IN THE SPTpol 100 SQUARE DEGREE SURVEY

Whitehorn

Natoli

Ade

et al. 2016

ApJ

View full text Add to dashboard Cite

The millimeter transient sky is largely unexplored, with measurements limited to follow-up of objects detected at other wavelengths. High-angular-resolution telescopes, designed for measurement of the cosmic microwave background (CMB), offer the possibility to discover new, unknown transient sources in this band-particularly the afterglows of unobserved gamma-ray bursts (GRBs). Here, we use the 10 m millimeter-wave South Pole Telescope, designed for the primary purpose of observing the CMB at arcminute and larger angular scales, to conduct a search for such objects. During the 2012-2013 season, the telescope was used to continuously observe a 100 deg 2 patch of sky centered at R.A. 23 h 30 m and decl. −55°using the polarization-sensitive SPTpol camera in two bands centered at 95 and 150 GHz. These 6000 hr of observations provided continuous monitoring for day-to month-scale millimeter-wave transient sources at the 10 mJy level. One candidate object was observed with properties broadly consistent with a GRB afterglow, but at a statistical significance too low (p = 0.01) to confirm detection.

show abstract

“…Searches of transients in radio archival observations or radio surveys (Levinson et al 2002;Gal-Yam et al 2006;Bannister et al 2011;Bell et al 2011;Bower and Saul 2011;Bower et al 2007Bower et al , 2010Croft et al 2010;Frail et al 2012;Carilli et al 2003;Matsumura et al 2009;Lazio et al 2010) set upper limits on the sky density of transients. Detection of radio transients is, however, only the first step towards the identification of OA, because many other astronomical objects can produce radio transients (see e.g.…”

Section: Present Limitsmentioning

confidence: 99%

GRB Orphan Afterglows in Present and Future Radio Transient Surveys

Ghirlanda

Burlon

Ghisellini

et al. 2014

Publ. Astron. Soc. Aust.

View full text Add to dashboard Cite

Orphan Afterglows (OA) are slow transients produced by Gamma Ray Bursts seen off-axis that become visible on timescales of days/years at optical/NIR and radio frequencies, when the prompt emission at high energies (X and γ rays) has already ceased. Given the typically estimated jet opening angle of GRBs θ jet ∼ 3 • , for each burst pointing to the Earth there should be a factor ∼ 700 more GRBs pointing in other directions. Despite this, no secure OAs have been detected so far. Through a population synthesis code we study the emission properties of the population of OA at radio frequencies. OAs reach their emission peak on year-timescales and they last for a comparable amount of time. The typical peak fluxes (which depend on the observing frequency) are of few μJy in the radio band with only a few OA reaching the mJy level. These values are consistent with the upper limits on the radio flux of SN Ib/c observed at late times. We find that the OA radio number count distribution has a typical slope −1.7 at high fluxes and a flatter (−0.4) slope at low fluxes with a break at a frequency-dependent flux. Our predictions of the OA rates are consistent with the (upper) limits of recent radio surveys and archive searches for radio transients. Future radio surveys like VAST/ASKAP at 1.4 GHz should detect ∼ 3 × 10 −3 OA deg −2 yr −1 , MeerKAT and EVLA at 8.4 GHz should see ∼ 3 × 10 −1 OA deg −2 yr −1 . The SKA, reaching the μJy flux limit, could see up to ∼ 0.2 − 1.5 OA deg −2 yr −1 . These rates also depend on the duration of the OA above a certain flux limit and we discuss this effect with respect to the survey cadence.

show abstract

THE ALLEN TELESCOPE ARRAY Pi GHz SKY SURVEY. I. SURVEY DESCRIPTION AND STATIC CATALOG RESULTS FOR THE BOÖTES FIELD

Cited by 30 publications

References 54 publications

Discovery of a Meter-Wavelength Radio Transient in the Swire Deep Field: 1046+59

Discovery of a Meter-Wavelength Radio Transient in the Swire Deep Field: 1046+59

MILLIMETER TRANSIENT POINT SOURCES IN THE SPTpol 100 SQUARE DEGREE SURVEY

GRB Orphan Afterglows in Present and Future Radio Transient Surveys

Contact Info

Product

Resources

About