AMICA, an astro-mapper for AMS

Monfardini, A.; Trampus, Paolo; Battiston, R.; Gargiulo, C.

doi:10.1016/j.astropartphys.2005.11.008

Cited by 6 publications

(6 citation statements)

References 10 publications

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“…A possible rebrightening is visible only in the IR, although a monotonic decay is not ruled out. A similar feature has been seen in the case of GRB 060206 (Monfardini et al 2006b). If real, it might indicate a second reverse shock emission, initiated by the 300-s flare.…”

Section: O N C L U S I O N Ssupporting

confidence: 80%

“…The significance is low and a monotonic decay is not ruled out. On the other hand, it is worth to point out that a similar feature has been detected at larger significance in the brighter GRB 060206 (Monfardini et al 2006b), in which case the R and i light curves could not be fitted with identical functions. If real, the rebrightening in the i band may de due to a second reverse shock, possibly initiated by the collision of the 300 s of the X-ray flare into the external medium.…”

Section: Afterglow Modelmentioning

confidence: 94%

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Anatomy of a dark burst - the afterglow of GRB 060108

Oates¹,

Mundell

Piranomonte

et al. 2006

Monthly Notices of the Royal Astronomical Society

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We present a multiwavelength study of GRB 060108 - the 100th gamma-ray burst discovered by Swift. The X-ray flux and light curve (three segments plus a flare) detected with the X-ray Telescope are typical of Swift long bursts.\ud \ud We report the discovery of a faint optical afterglow detected in deep BVRi'-band imaging obtained with the Faulkes Telescope North beginning 2.75 min after the burst. The afterglow is below the detection limit of the Ultraviolet/Optical Telescope within 100 s of the burst, while is evident in K-band images taken with the United Kingdom Infrared Telescope 45 min after the burst. The optical light curve is sparsely sampled. Observations taken in the R and i' bands can be fitted either with a single power-law decay in flux, F(t) ~ t-α where α = 0.43 +/- 0.08, or with a two-segment light curve with an initial steep decay α1 < 0.88 +/- 0.2, flattening to a slope α2 ~ 0.31 +/- 0.12. A marginal evidence for rebrightening is seen in the i' band.\ud \ud Deep R-band imaging obtained ~12 d post-burst with the Very Large Telescope reveals a faint, extended object (R ~ 23.5mag) at the location of the afterglow. Although the brightness is compatible with the extrapolation of the slow decay with index α2, significant flux is likely due to a host galaxy. This implies that the optical light curve had a break before 12 d, akin to what observed in the X-rays.\ud \ud We derive the maximum photometric redshift z < 3.2 for GRB 060108. We find that the spectral energy distribution at 1000 s after the burst, from the optical to the X-ray range, is best fitted by a simple power law, Fν ~ ν-β, with βOX = 0.54 and a small amount of extinction. The optical to X-ray spectral index (βOX) confirms GRB 060108 to be one of the optically darkest bursts detected. Our observations rule out a high redshift as the reason for the optical faintness of GRB 060108. We conclude that a more likely explanation is a combination of an intrinsic optical faintness of the burst, a hard optical to X-ray spectrum and a moderate amount of extinction in the host galaxy

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Section: O N C L U S I O N Ssupporting

confidence: 80%

Section: Afterglow Modelmentioning

confidence: 94%

Anatomy of a dark burst - the afterglow of GRB 060108

Oates¹,

Mundell

Piranomonte

et al. 2006

Monthly Notices of the Royal Astronomical Society

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“…Therefore, either version (5) of the former scenario, in which the X-ray and the optical afterglows are due to separate jet components, or the latter scenario are preferable for this event. A recent Swift burst, GRB 060206, showed a late-time steepening of the optical light curve, but no break in the X-ray light curve at the same time (Monfardini et al 2006), which also lends support to version (5) of the former scenario, in which the X-ray and the optical afterglows are due to separate jet components.…”

Section: Implications Of No Jet Break Feature In the X-ray Bandmentioning

confidence: 57%

SwiftDiscovery of Gamma‐Ray Bursts without a Jet Break Feature in Their X‐Ray Afterglows

Sato

Yamazaki

Ioka

et al. 2007

ApJ

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We analyze Swift gamma-ray bursts (GRBs) and X-ray afterglows for three GRBs with spectroscopic redshift determinations -GRB 050401, XRF 050416a, and GRB 050525a. We find that the relation between spectral peak energy and isotropic energy of prompt emissions (the Amati relation) is consistent with that for the bursts observed in pre-Swift era. However, we find that the X-ray afterglow -2lightcurves, which extend up to 10-70 days, show no sign of the jet break that is expected in the standard framework of collimated outflows. We do so by showing that none of the X-ray afterglow lightcurves in our sample satisfies the relation between the spectral and temporal indices that is predicted for the phase after jet break. The jet break time can be predicted by inverting the tight empirical relation between the peak energy of the spectrum and the collimation-corrected energy of the prompt emission (the Ghirlanda relation). We find that there are no temporal breaks within the predicted time intervals in X-ray band. This requires either that the Ghirlanda relation has a larger scatter than previously thought, that the temporal break in X-rays is masked by some additional source of X-ray emission, or that it does not happen because of some unknown reason.

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“…Therefore, a better understanding of high redshift cluster properties can only be achieved via high resolution tSZ observations [10]. The NIKA camera ( [9]), installed at the 30 m IRAM telescope in Pico Veleta, was a pioneer in this respect as will be shown in this paper. NIKA [9,11] was a dual band millimeter intensity and polarization camera operated at 150 and 260 GHz and installed permanently at the IRAM 30-m telescope from 2013 to 2015.…”

Section: Introductionmentioning

confidence: 98%

“…The NIKA camera ( [9]), installed at the 30 m IRAM telescope in Pico Veleta, was a pioneer in this respect as will be shown in this paper. NIKA [9,11] was a dual band millimeter intensity and polarization camera operated at 150 and 260 GHz and installed permanently at the IRAM 30-m telescope from 2013 to 2015. The NIKA camera (see Figure 2) was made of two arrays of Kinetic Inductance Detectors (KIDs) cooled down to 100 mK via a 3 He- 4 He dilution cryostat and instrumented via a dedicated readout electronics [13,14].…”

Section: Introductionmentioning

confidence: 99%

NIKA: a mm camera for Sunyaev-Zel’dovich science in clusters of galaxies

et al. 2020

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Clusters of galaxies, the largest bound objects in the Universe, constitute a cosmological probe of choice, which is sensitive to both dark matter and dark energy. Within this framework, the Sunyaev-Zel'dovich (SZ) effect has opened a new window for the detection of clusters of galaxies and for the characterization of their physical properties such as mass, pressure and temperature. NIKA, a KID-based dual band camera installed at the IRAM 30-m * telescope, was particularly well adapted in terms of frequency, angular resolution, field-of-view and sensitivity, for the mapping of the thermal and kinetic SZ effect in high-redshift clusters. In this paper, we present the NIKA cluster sample and a review of the main results obtained via the measurement of the SZ effect on those clusters: reconstruction of the cluster radial pressure profile, mass, temperature and velocity.

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AMICA, an astro-mapper for AMS

Cited by 6 publications

References 10 publications

Anatomy of a dark burst - the afterglow of GRB 060108

Anatomy of a dark burst - the afterglow of GRB 060108

SwiftDiscovery of Gamma‐Ray Bursts without a Jet Break Feature in Their X‐Ray Afterglows

NIKA: a mm camera for Sunyaev-Zel’dovich science in clusters of galaxies

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