J/MNRAS/498/5720 Extended Breakthrough Listen sample (Wlodarczyk-Sroka+, 2020) ================================================================================ Extending the Breakthrough Listen nearby star survey to other stellar objects in the field. Wlodarczyk-Sroka B.S., Garrett M.A., Siemion A.P.V. =2020MNRAS.498.5720W (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Surveys ; Proper motions ; Parallaxes, trigonometric ; Stars, distances ; Radial velocities Keywords: astronomical instrumentation - methods and techniques - astrometry - stars: general - radio continuum: general Abstract: We extend the source sample recently observed by the Breakthrough Listen Initiative by including additional stars (with parallaxes measured by Gaia) that also reside within the FWHM of the GBT and Parkes radio telescope target fields. These stars have estimated distances as listed in the extensions of the Gaia DR2 catalogue. Enlarging the sample from 1327 to 288315 stellar objects permits us to achieve substantially better Continuous Waveform Transmitter Rate Figures of Merit (CWTFM) than any previous analysis, and allows us to place the tightest limits yet on the prevalence of nearby high-duty-cycle extraterrestrial transmitters. The results suggest <~0.0660(+0.0004,-0.0003)% of stellar systems within 50 pc host such transmitters (assuming an EIRP>~10^13^W) and <~0.039(+0.004,-0.008)% within 200pc (assuming an EIRP>~2.5*10^14^W). We further extend our analysis to much greater distances, though we caution that the detection of narrow-band signals beyond a few hundred pc may be affected by interstellar scintillation. The extended sample also permits us to place new constraints on the prevalence of extraterrestrial transmitters by stellar type and spectral class. Our results suggest targeted analyses of SETI radio data can benefit from taking into account the fact that in addition to the target at the field centre, many other cosmic objects reside within the primary beam response of a parabolic radio telescope. These include foreground and background galactic stars, but also extragalactic systems. With distances measured by Gaia, these additional sources can be used to place improved limits on the prevalence of extraterrestrial transmitters, and extend the analysis to a wide range of cosmic objects. Description: Using the target sample of Price et al. (2020AJ....159...86P), the Gaia DR2 catalogue and its extensions were probed to compile a list of stars contained within the fields of view studied by Price et al. (2020AJ....159...86P). 288315 unique sources were observed by the three radio telescope receivers used (GBT L-band, GBT S-band and Parkes 10-cm), across 356616 observations (210146 with the GBT at L-band, 89654 with the GBT at S-band, and 56816 with Parkes). Minimum detectable Equivalent Isotropic Radiated Power values are presented as calculated from the source position in the beam (by applying a Gaussian sensitivity function) and the source estimated distance taken from Bailer-Jones et al. (2018AJ....156...58B, Cat. I/347). File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file catalog.dat 631 356616 Table of the 288315 stars included as part of our extension of the original Breakthrough Listen sample of Price et al. (2020AJ....159...86P) -------------------------------------------------------------------------------- See also: I/345 : Gaia DR2 (Gaia Collaboration, 2018) I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018) Byte-by-byte Description of file: catalog.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 19 I19 --- GaiaDR2 Gaia DR2 unique source identifier 21- 42 F22.18 deg RAdeg Right ascension (ICRS) at Ep=2015.5 44- 64 F21.19 mas e_RAdeg Standard error of right ascension 66- 88 E23.19 deg DEdeg Declination (ICRS) at Ep=2015.5 90-109 F20.18 mas e_DEdeg Standard error of declination 111-133 E23.19 mas Plx Parallax 135-147 E13.9 --- RPlx Parallax divided by its error 149-170 E22.19 mas/yr pmRA Proper motion in right ascension direction, pmRA*cosDE 172-191 F20.18 mas/yr e_pmRA Standard error of proper motion in right ascension direction 193-214 E22.19 mas/yr pmDE Proper motion in declination direction 216-235 F20.18 mas/yr e_pmDE Standard error of proper motion in declination direction 237-246 F10.7 mag Gmag G-band mean magnitude 248-260 E13.10 mag BP-RP ? BP-RP colour index 262-283 F22.17 km/s RV ? Radial velocity 285-304 F20.17 km/s e_RV ? Radial velocity error 306-314 F9.4 K Teff ? Source effective temperature 316-339 A24 --- Target Target designation 341-359 F19.15 deg RATdeg Target right ascension (ICRS) at Ep=2015.5 361-378 F18.14 deg DETdeg Target declination (ICRS) at Ep=2015.5 380-387 F8.4 mas PlxT Target parallax 389-397 F9.3 mas/yr pmRAT Target proper motion in right ascension direction, pmRA*cosDE 399-407 F9.3 mas/yr pmDET Target proper motion in declination direction 409-416 F8.3 km/s RVT Target radial velocity 418-436 F19.14 pc rest Estimated distance (1) 438-456 F19.14 pc b_rest Lower bound on the confidence interval of the estimated distance (1) 458-477 F20.14 pc B_rest Upper bound on the confidence interval of the estimated distance (1) 479-497 F19.12 pc rlen Length scale used in the prior for the distance estimation (1) 499-522 A24 --- InstT Telescopes used to observe the target 524-535 A12 --- InstS Telescope used to observe individual source in a particular pointing 537-539 F3.1 arcmin FWHM Full-width at half-maximum of receiver primary beam 541-561 E21.17 deg Offset-deg Total angular offset of source from target 563-583 E21.17 arcmin Offset-arcmin Total angular offset of source from target 585-602 F18.16 --- TelResGaus Sensitivity response of telescope at offset (2) 604-625 E22.17 W min-detec-EIRP Minimum detectable Equivalent Isotropic Radiated Power for source 627-631 A5 --- Price-target? [false/true ] In original target sample of Price et al. (2020AJ....159...86P) ?(3) -------------------------------------------------------------------------------- Note (1): Estimated distance values determined the catalogue presented by Bailer-Jones et al. (2018AJ....156...58B). Note (2): Determined from a Gaussian fit to the angular offset of the source from the pointing target. Note (3): Flag as follows: true = source featured in original target sample of Price et al. (2020AJ....159...86P) false = source featured in extended sample presented in this paper. -------------------------------------------------------------------------------- Acknowledgements: Bart S. Wlodarczyk-Sroka, bart.wlodarczyk-sroka(at)postgrad.manchester.ac.uk References: Arenou et al., 2018A&A...616A..17A, Cat. I/345 Astropy Collaboration et al., 2018AJ....156..123A Astropy Collaboration et al., 2013A&A...558A..33A Backus P. R., Project Phoenix Team, 2002, Astronomical Society of the PacificConference Series, Vol. 278, Project Phoenix: SETI Observations from 1200 to1750 MHz with the Upgraded Arecibo Telescope, Stanimirovic S., AltschulerD., Goldsmith P., Salter C., eds., pp. 525-527 2002ASPC..278..525B Bailer-Jones et al., 2018AJ....156...58B, Cat. I/347 Cordes et al., 1997ApJ...487..782C Enriquez et al., 2017ApJ...849..104E Gaia Collaboration et al., 2018A&A...616A..10G, Cat. I/345 Gaia Collaboration et al., 2018A&A...616A...1G, Cat. I/345 Gaia Collaboration et al., 2016A&A...595A...1G, Cat. I/337 Garrett M. A., 2018, arXiv e-prints, arXiv:1810.07235, 2018arXiv181007235G Gertz J., 2020, arXiv e-prints, arXiv:2001.00673, 2020arXiv200100673G Gray & Mooley, 2017AJ....153..110G Hickish et al., 2019, 2019BAAS...51g.269H Isaacson et al., 2017PASP..129e4501I, Cat. J/PASP/129/e4501 Kozakis et al.. 2020ApJ...894L...6K Lacki et al., 2020, arXiv e-prints, arXiv:2006.11304, 2020arXiv200611304L van Leeuwen, 2007A&A...474..653V, Cat. I/311 Luri et al., 2018A&A...616A...9L, Cat. I/345 Perryman et al., 1997A&A...323L..49P Price et al., 2020AJ....159...86P Siemion et al., 2013ApJ...767...94S, Cat. J/ApJ/767/94 Taylor, 2005, in Astronomical Society of the Pacific Conference Series, Vol. 347, Astronomical Data Analysis Software and Systems XIV, Shopbell P.,Britton M., Ebert R., eds., p. 29, 2005ASPC..347...29T Worden et al., 2017, Acta Astronautica, 139, 98, 2017AcAau.139...98W ================================================================================ (End) Patricia Vannier [CDS] 02-Sep-2020