J/A+A/686/A56 GRB afterglow/supernova/host observations (Kann+, 2024)
Fires in the deep: The luminosity distribution of early-time gamma-ray-burst
afterglows in light of the Gamow Explorer sensitivity requirements.
Kann D.A., White N.E., Ghirlanda G., Oates S.R., Melandri A., Jelinek M.,
de Ugarte Postigo A., Levan A.J., Martin-Carrillo A., Paek G.S.-H., Izzo L.,
Blazek M., Thoene C.C., Aguei Fernandez J.F., Salvaterra R., Tanvir N.R.,
Chang T.-C., O'Brien P., Rossi A., Perley D.A., Im M., Malesani D.B.,
Antonelli A., Covino S., Choi C., D'Avanzo P., D'Elia V., Dichiara S.,
Fausey H.M., Fugazza D., Gomboc A., Gorski K.M., Granot J., Guidorzi C.,
Hanlon L., Hartmann D.H., Hudec R., Jun H.D., Kim J., Kim Y., Klose S.,
Kluzniak W., Kobayashi S., Kouveliotou C., Lidz A., Marongiu M.,
Martone R., Meintjes P., Mundell C.G., Murphy D., Nalewajko K., Park W.-K.,
Szecsi D., Smith R.J., Stecklum B., Steele I.A., Strobl J., Sung H.-I-,
Updike A., Urata Y., van der Horst A.J.
<Astron. Astrophys. 686, A56 (2024)>
=2024A&A...686A..56K 2024A&A...686A..56K (SIMBAD/NED BibCode)
ADC_Keywords: GRB ; Photometry, infrared ; Optical ; Ultraviolet
Keywords: methods: observational - space vehicles -
space vehicles: instruments - techniques: photometric -
gamma-ray burst: general - dark ages, reionization, first stars
Abstract:
Gamma-ray bursts (GRBs) are ideal probes of the Universe at high
redshift (z), pinpointing the locations of the earliest star-forming
galaxies and providing bright backlights with simple featureless
power-law spectra that can be used to spectrally fingerprint the
intergalactic medium and host galaxy during the period of
reionization. Future missions such as Gamow Explorer (hereafter Gamow)
are being proposed to unlock this potential by increasing the rate of
identification of high-z (z>5) GRBs in order to rapidly trigger
observations from 6-10m ground telescopes, the James Webb Space
Telescope (JWST), and the upcoming Extremely Large Telescopes (ELTs).
Gamow was proposed to the NASA 2021 Medium-Class Explorer (MIDEX)
program as a fast-slewing satellite featuring a wide-field lobster-eye
X-ray telescope (LEXT) to detect and localize GRBs with arcminute
accuracy, and a narrow-field multi-channel photo-z infrared telescope
(PIRT) to measure their photometric redshifts for >80% of the LEXT
detections using the Lyman- dropout technique. We use a large sample
of observed GRB afterglows to derive the PIRT sensitivity requirement.
We compiled a complete sample of GRB optical-near-infrared
(optical-NIR) afterglows from 2008 to 2021, adding a total of 66 new
afterglows to our earlier sample, including all known high-z GRB
afterglows. This sample is expanded with over 2837 unpublished data
points for 40 of these GRBs.We performed full light-curve and
spectral-energy-distribution analyses of these afterglows to derive
their true luminosity at very early times. We compared the high-z
sample to the comparison sample at lower redshifts. For all the light
curves, where possible, we determined the brightness at the time of
the initial finding chart of Gamow, at different high redshifts and in
different NIR bands. This was validated using a theoretical approach to
predicting the afterglow brightness. We then followed the evolution of
the luminosity to predict requirements for groundand space-based
follow-up. Finally, we discuss the potential biases between known GRB
afterglow samples and those to be detected by Gamow.
We find that the luminosity distribution of high-z GRB afterglows is
comparable to those at lower redshift, and we therefore are able to
use the afterglows of lower-z GRBs as proxies for those at high z. We
find that a PIRT sensitivity of 15uJy (21mag AB) in a 500s exposure
simultaneously in five NIR bands within 1000s of the GRB trigger will
meet the Gamow mission requirements. Depending on the z and NIR band,
we find that between 75% and 85% of all afterglows at z>5 will be
recovered by Gamow at 5σ detection significance, allowing the
determination of a robust photo-z. As a check for possible
observational biases and selection effects, we compared the results with
those obtained through population-synthesis models, and find them to
be consistent.
Gamow and other high-z GRB missions will be capable of using a
relatively modest 0.3m onboard NIR photo-z telescope to rapidly
identify and report high-z GRBs for further follow-up by larger
facilities, opening a new window onto the era of reionization and the
high-redshift Universe.
Description:
We took a large sample of GRB optical and NIR afterglows
from 2008 to 2021 and used them to predict the expected afterglow
brightness verses time for GRBs from high-z (z>5).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
sources.dat 36 40 GRB list
tableb1.dat 84 2844 GRB afterglow/supernova/host observations
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Byte-by-byte Description of file: sources.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name GRB name
14- 15 I2 h RAh Simbad right ascension (J2000)
17- 18 I2 min RAm Simbad right ascension (J2000)
20- 24 F5.2 s RAs Simbad right ascension (J2000)
26 A1 --- DE- Simbad declination sign (J2000)
27- 28 I2 deg DEd Simbad declination (J2000)
30- 31 I2 arcmin DEm Simbad declination (J2000)
33- 36 F4.1 arcsec DEs Simbad declination (J2000)
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 -- Name GRB name
14- 24 F11.6 d Dt Time interval Δt (1)
26 A1 --- l_mag Limit flag on mag
27- 32 F6.3 mag mag ? Magnitude in Filter (2)
33 A1 --- n_mag [R] R for Reference
35- 39 F5.3 mag E_mag ? Upper value of magnitude error
41 A1 --- --- [-]
42- 46 F5.3 mag e_mag ? Lower value of magnitude error
49- 53 A5 --- Filter Filter
58- 84 A27 --- Tel Telescope/Instrument
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Note (1): Midtimes are derived logarithmically.
t=10([log(t1-t0)+log(t2-t0_)]/2)^, hereby t1.2 are the absolute
start and stop times, and t0 is the GRB trigger time.
Note (2): All data are in AB magnitudes and not corrected for Galactic
foreground extinction.
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Acknowledgements:
Nicholas White, newhite(at)email.gwu.edu
(End) Patricia Vannier [CDS] 28-Feb-2024