English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

GRBs generate an afterglow emission that can be detected from radio to X-raysduring days, or even weeks after the initial explosion. The peak of thisemission crosses the mm/submm range during the first hours to days, makingtheir study in this range crucial for constraining the models. Observationshave been limited until now due to the low sensitivity of the observatories inthis range. We present observations of 10 GRB afterglows obtained from APEX andSMA, as well as the first detection of a GRB with ALMA, and put them intocontext with all the observations that have been published until now in thespectral range that will be covered by ALMA. The catalogue of mm/submmobservations collected here is the largest to date and is composed of 102 GRBs,of which 88 had afterglow observations, whereas the rest are host galaxysearches. With our programmes, we contributed with data of 11 GRBs and thediscovery of 2 submm counterparts. In total, the full sample, including datafrom the literature, has 22 afterglow detections with redshift ranging from0.168 to 8.2. GRBs have been detected in mm/submm wavelengths with peakluminosities spanning 2.5 orders of magnitude, the most luminous reaching10^33erg s^-1 Hz^-1. We observe a correlation between the X-ray brightness at0.5 days and the mm/submm peak brightness. Finally we give a rough estimate ofthe distribution of peak flux densities of GRB afterglows, based on the currentmm/submm sample. Observations in the mm/submm bands have been shown to becrucial for our understanding of the physics of GRBs, but have until now beenlimited by the sensitivity of the observatories. With the start of theoperations at ALMA, the sensitivity will be increased by more than an order ofmagnitude. Our estimates predict that, once completed, ALMA will detect up to98% of the afterglows if observed during the passage of the peak synchrotronemission.

Pre-ALMA observations of GRBs in the mm/submm range