A New System of Faint Near-Infrared Standard Stars

Persson, S. E.; Murphy, D. C.; Krzemiński, W.; Roth, M.; Rieke, M. J.

doi:10.1086/300607

Cited by 777 publications

(917 citation statements)

References 14 publications

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“…These standards and thus the near-IR measurements reported in the present paper are based on the JHKs photometric system introduced by Persson et al (1998). The derived zero-point error was 0.03 mag in both the J and Ks bands.…”

Section: Photometric Calibrationmentioning

confidence: 64%

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Gorosabel¹,

Fynbo²,

Hjorth

et al. 2002

A&A

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Abstract.We report the discovery of the optical and near-infrared counterparts to GRB 001011. The GRB 001011 error box determined by Beppo-SAX was simultaneously imaged in the near-infrared by the 3.58-m New Technology Telescope and in the optical by the 1.54-m Danish Telescope ∼8 hr after the gamma-ray event. Here we implement the colour-colour discrimination technique proposed by Rhoads (2001) and extend it using near-IR data as well. We present the results provided by an automatic colour-colour discrimination pipe-line developed to discern the different populations of objects present in the GRB 001011 error box. Our software revealed three candidates based on single-epoch images. Second-epoch observations carried out ∼3.2 days after the burst revealed that the most likely candidate had faded, thus identifying it with the counterpart to the GRB. In deep R-band images obtained 7 months after the burst a faint (R = 25.38 ± 0.25) elongated object, presumably the host galaxy of GRB 001011, was detected at the position of the afterglow. The GRB 001011 afterglow is the first discovered with the assistance of colour-colour diagram techniques. We discuss the advantages of using this method and its application to error boxes determined by future missions.

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Section: Photometric Calibrationmentioning

confidence: 64%

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Gorosabel¹,

Fynbo²,

Hjorth

et al. 2002

A&A

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show abstract

“…Bad pixels were replaced by the median of surrounding pixels. The absolute calibration of the images was set by observing HST IR standard stars (Persson et al 1998). On 19 December we used SJ9134 and SJ9138, for which we adopted magnitudes of 11.596 and 10.982 in the CH 4 bands, respectively.…”

Section: Data Acquisition and Image Processingmentioning

confidence: 99%

Keck observations of the 2002–2003 jovian ring plane crossing

Pater¹,

Showalter²,

Macintosh³

2008

Icarus

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We present new observations of Jupiter's ring system at a wavelength of 2.2 µm obtained with the 10-m W. M. Keck telescopes on three nights during a ring plane crossing: UT 19 December 2002, and 22 and 26 January 2003. We used conventional imaging, plus adaptive optics on the last night. Here we present detailed radial profiles of the main ring, halo and gossamer rings, and interpret the data together with information extracted from radio observations of Jupiter's synchrotron radiation. The main ring is confined to a 800-km-wide annulus between 128,200 and 129,000 km, with a ∼ 5000 km extension on the inside. The normal optical depth is 8 × 10 −6 , 15% of which is provided by bodies with radii a > ∼ 5 cm. These bodies are as red as Metis. Half the optical depth, τ ≈ 4 × 10 −6 , is attributed to micron-sized dust, and the remaining τ ≈ 3 × 10 −6 to grains tens to hundreds of µm in size. The inward extension consists of micron-sized (a < ∼ 10 µm ) dust, which probably migrates inward under Poynting-Robertson drag. The inner limit of this extension falls near the 3:2 Lorentz resonance (at orbital radius r = 122, 400 km), and coincides with the outer limit of the halo. The gossamer rings appear to be radially confined, rather than broad sheets of material. The Amalthea ring is triangularly shaped, with a steep outer dropoff over ∼5000 km, extending a few 1000 km beyond the orbit of Amalthea, and a more gradual inner dropoff over 15,000-20,000 km. The inner edge is near the location of the synchronous orbit. The optical depth in the Amalthea ring is ∼ 5×10 −7 , up to 20% of which is comprised of macroscopic material. The optical depth in the Thebe ring is a factor of 3 smaller.

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“…In DP02, this problem was tackled by calibrating Io's flux density in the SCAM (slit camera) images, by observing the G4 infrared standard star SJ9182 (Persson et al 1998). Io's continuum level in the reduced spectra was then scaled to In this paper we directly calibrated the stellar spectra using 2MASS.…”

Section: Observationsmentioning

confidence: 99%

Temporal behavior of the SO 1.707 μm ro-vibronic emission band in Io's atmosphere

Laver¹,

Pater²,

Roe³

et al. 2007

Icarus

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We report observations of the ro-vibronic a 1 ∆ → X 3 Σ − transition of SO at 1.707 µm on Io. These data were taken while Io was eclipsed by Jupiter, on four nights between July 2000 and March 2003. We analyze these results in conjunction with a previously published night to investigate the temporal behavior of these emissions. The observations were all conducted using the near-infrared spectrometer NIRSPEC on the W.M. Keck II telescope. The integrated emitted intensity for this band varies from 0.8 x 10 27 to 2.4 x 10 27 photons/sec, with a possible link to variations in Loki's infrared brightness. The band-shapes imply rotational temperatures of 550-1000K for the emitting gas, lending further evidence to a volcanic origin for sulfur monoxide. An attempt to detect the B 1 Σ → X 3 Σ − transition of SO at 0.97 µm was unsuccessful; simultaneous detection with the 1.707 µm band would permit determination of the SO column abundance.

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A New System of Faint Near-Infrared Standard Stars

Cited by 777 publications

References 14 publications

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Keck observations of the 2002–2003 jovian ring plane crossing

Temporal behavior of the SO 1.707 μm ro-vibronic emission band in Io's atmosphere

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