Teaching Freshmen to Read

Pooley, Robert C.; Altick, Richard D.

doi:10.2307/372828

Cited by 3 publications

(5 citation statements)

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“…The low-frequency spectrum below ν m (F ν ∝ ν 1/3 ) is in agreement with the expected tail of the synchrotron radiation plus a self absorption that becomes important below a critical frequency ν a ∼ 13 GHz, taking into account that F ν ∝ ν 1.4 in the range 4. 86-8.46 GHz (Frail et al 1999), deviating from F ν ∝ ν 1/3 as seen for 15 GHz < ν < 100 GHz (Pooley et al 1999). Much more accurate estimates for ν a and ν m are given by Galama et al (2000a).…”

Section: The Multiwavelength Spectrum On Dec 120mentioning

confidence: 94%

“…Coincident (within errors) with the location of optical and radio afterglows, Shepherd et al (1999) detected at millimeter wavelengths the brightest afterglow of a GRB reported so far. At 15 GHz and 240 GHz, the GRB 991208 afterglow was observed at Ryle (Pooley et al 1999) and Pico Veleta (Bremer et al 1999a,b), respectively.…”

Section: The Optical Afterglowmentioning

confidence: 99%

“…Circles are the extrapolation of the BV RI measurements following the power-law derived in this paper. The diamond is the Pico Veleta measurement (Bremer et al 1999a,b), the square is the OVRO data point (Shepherd 1999), the triangle-up is the flux density obtained at the Ryle telescope (Pooley et al 1999) and the triangles-down are the VLA data points (Frail et al 1999, Hurley et al 2000. The correction for galactic extinction has been considered taking into account E(B-V) = 0.016 from (Schlegel et al 1998).…”

Section: The Multiwavelength Spectrum On Dec 120mentioning

confidence: 99%

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The extraordinarily bright optical afterglow of GRB 991208 and its host galaxy

Castro‐Tirado

Соколов

Gorosabel

et al. 2001

A&A

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Broad-band optical observations of the extraordinarily bright optical afterglow of the intense gamma-ray burst GRB 991208 started ∼ 2.1 days after the event and continued until 4 Apr 2000. The flux decay constant of the optical afterglow in the R-band is −2.30 ± 0.07 up to ∼ 5 days, which Send offprint requests to: A. J. Castro-Tirado (ajct@laeff.esa.es)is very likely due to the jet effect, and after that it is followed by a much steeper decay with constant −3.2 ± 0.2, the fastest one ever seen in a GRB optical afterglow. A negative detection in several all-sky films taken simultaneously to the event, that otherwise would have reached naked eye brightness, implies either a previous additional break prior to ∼ 2 days after the 2 A. J. Castro-Tirado et al.:The extraordinarily bright optical afterglow of GRB 991208.

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Section: The Multiwavelength Spectrum On Dec 120mentioning

confidence: 94%

Section: The Optical Afterglowmentioning

confidence: 99%

Section: The Multiwavelength Spectrum On Dec 120mentioning

confidence: 99%

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The extraordinarily bright optical afterglow of GRB 991208 and its host galaxy

Castro‐Tirado

Соколов

Gorosabel

et al. 2001

A&A

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“…GRB 991208 has been no less interesting at radio wavelengths. It has the brightest radio afterglow detected to date and consequently it has been detected and is well-studied between 1 GHz and 350 GHz (Pooley 1999;Shepherd et al 1999;Bremer et al 1999).…”

Section: Observations With Nrao Very Large Arraymentioning

confidence: 99%

Interplanetary Network Localization of GRB 991208 and the Discovery of its Afterglow

Hurley

Cline

Mazets

et al. 2000

The Astrophysical Journal

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The extremely energetic (∼10 Ϫ4 ergs cm Ϫ2 ) gamma-ray burst (GRB) of 1999 December 8 was triangulated to an ∼14 arcmin 2 error box ∼1.8 days after its arrival at Earth with the third interplanetary network (IPN), which consists of the Ulysses, Near-Earth Asteroid Rendezvous, and Wind spacecraft. Radio observations with the Very Large Array ∼2.7 days after the burst revealed a bright fading counterpart whose position is consistent with that of an optical transient source with a redshift of 0.707. We present the time history, peak flux, fluence, and refined 1.3 arcmin 2 error box of this event and discuss its energetics. This is the first time that a counterpart has been found for a GRB localized only by the IPN.

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“…This source had a rising spectral index. A few days after the burst, the source was found to have fluxes of a couple of mJy from 15 to 240 GHz using the Ryle Telescope (Pooley 1999a), Owens Valley Millimeter Array (Shepherd et al 1999), and IRAM (Bremer et al 1999). An optical transient was also found (Castro-Tirado et al 1999;Stecklum et al 1999) whose optical flux decayed following a power law ∝ t −δ with a steep slope δ = 2.3 ± 0.07 for the first ∼5 days, breaking to an even faster δ = 3.2 ± 0.2 .…”

Section: Grb 991208mentioning

confidence: 99%

SCUBA Sub-Millimeter Observations of Gamma-Ray Bursters

Smith¹,

Tilanus²,

Wijers³

et al. 2003

AIP Conference Proceedings

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Abstract. We discuss our ongoing program of Target of Opportunity sub-millimeter observations of gamma-ray bursts (GRBs) using the Sub-millimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT). Sub-millimeter observations of the early afterglows are of interest because this is where the emission peaks in some bursts in the days to weeks following the burst. Of increasing interest is to look for underlying quiescent sub-millimeter sources that may be dusty star-forming host galaxies. In this paper, we present observations of GRB 991208, 991216, 000301C, 000630, 000911, and 000926. For all these bursts, any sub-millimeter emission is consistent with coming from the afterglow. This means that we did not conclusively detect quiescent sub-millimeter counterparts to any of the bursts that were studied from 1997 through 2000. The inferred star formation rates (M ≥ 5 M ) are typically ∼ <300 M yr −1 . If GRBs are due to the explosions of high-mass stars, this may indicate that the relatively small population of extremely luminous dusty galaxies does not dominate the total star formation in the universe at early epochs. Instead, the GRBs may be predominantly tracing slightly lower luminosity galaxies. The optical faintness of some host galaxies is unlikely to be explained as due to dust absorption in the host.

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Teaching Freshmen to Read

Cited by 3 publications

References 0 publications

The extraordinarily bright optical afterglow of GRB 991208 and its host galaxy

The extraordinarily bright optical afterglow of GRB 991208 and its host galaxy

Interplanetary Network Localization of GRB 991208 and the Discovery of its Afterglow

SCUBA Sub-Millimeter Observations of Gamma-Ray Bursters

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