1. A Proposed Collaboration Between LIGO-Virgo and Swift to Improve the Chances to Detect Gravitational Waves from Core Collapse Supernovae Kiranjyot (Jasmine) Gill, 1 Dr. Michele Zanolin 1 With support from Marek Szczepanczyk 1 1 Physics Department, Embry-Riddle Aeronautical University, Prescott, AZ XRT in Contrast with Optical Observation Future Directions Swift X-ray Telescope (XRT) Overview Physical Assumptions and Constraints Acknowledgements Table 1 Improvements Provided by Swift XRT ObjectAngular SizeDistance Messier 8211.2 ‘ x 4.3 ‘3.5-3.8 Mpc NGC 456515.9’ x 1.85’16.2 Mpc NGC 63571 degree x 1 degree48504.34 pc Canis Major Dwarf Galaxy 12 degrees x 12 degrees 8584.839 pc Support provided by: LVC Organization ERAU URI Abstract References [1] arXiv:0802.1712v2 [2] arXiv:1306.0559v1  Bursts observed by the Beppo-SAX X-ray telescopes detect GRBs within 6-8 hours by observing the fading X-ray afterglows.  By the time the observation is made however, the intensity has dropped by 4-5 orders of magnitude.  The Swift XRT will begin observations before the GRB ends in many cases, and will fill in the large time gap during which the Lorentz factor of the relativistic blast wave changes.  X-ray info gives better time constraints on the emission of gravitational waves (GW)  From the usage of the XRT, there will be a theorized lower false alarm rate associated with the data collection. [2]  Swift XRT = X-ray CCD imaging spectrometer designed to measure the position, spectrum, and brightness of gamma-ray bursts (GRBs) and afterglows over a wide dynamic range covering more than 7 orders of magnitude in flux.  Field of View (‘) = 23.6 x 23.6  +70 short gamma-ray bursts (GRBs) found & sizable fraction = X- ray & optical afterglows; a few have been detected in the radio spectrum.  Discovered # of GRBs with their associated transients through their XRT X-Ray light curves. [1]  Stellar collapses generating a supernova explosion mechanism itself presents an unlikely possibility.  But, also rare due to intergalactic events such as the absorption of optical emissions from events such as dust obscuration, which not only prevents onset detection but interferes with any possible data collection.  Currently only 20% [2] of Supernovae (SNe) may be observed using only the optical range  The X-ray emissions within 20 Mpc will not be absorbed and thus is correlated to GWs produced in < 20 Mpc. [1]  increase detection efficiency of nearby supernovas  surpass 20% [2] factor provided by the optical detector capabilities The Core-Collapse supernovae (CCSNe) mark the dynamic and explosive end of the lives of massive stars. The mysterious mechanism behind CCSNe explosions could be explained by detecting the corresponding gravitational wave (GW) emissions by the laser interferometer gravitational wave observatory, LIGO. GWs are extremely hard to detect because they are weak signals in a floor of instrument noise. Optical observations of CCSNe are already used in coincidence with LIGO data, as a hint of the times when to search for the emission of GWs. More of these hints would be very helpful. For the first time in history a Harvard group has observed X-ray transients in coincidence with optical CCSNe. This discovery has proven that even if a supernova had its light absorbed with dust, X-ray transients that are more penetrating, and thus could be used as a hint on when to search for GWs. The SWIFT satellite can monitor galaxies with an X-ray probe. SWIFT is interested in collaborating with LIGO. The main goal of this project will be to quantify the benefits for LIGO by using the SWIFT satellite to monitor galaxies within 20 Mega parsecs from Earth, because beyond that assumed distance LIGO is incapable of producing a sensitivity that would allow a GW detection from CCSNe. Sampled LIGO Interferometer Noise  Data base search to evaluate an observational rate for different survey and bands  Evaluation of E&M information valuable for the GW-triggered search and the comparison with the theoretical population synthesis expectation  LIGO-Virgo-SWIFT Conference; Presentation; Discussion and Evaluation of Swift Satellite usage  Compilation of two documents; one focusing on the Memorandum of Understanding issued between the LIGO-Virgo and Swift collaborations while the second paper focuses on the First Targeted Search for GWB from SN in Coincidence with X-ray observations from Swift  B= 10^{-20.5 – A/2.5}  Where B is the blue luminosity of each given galaxy, and A is the absolute magnitude of each given galaxy. Blue Luminosity units: erg (which is 10 -7 J) s -1 Absolute Magnitude units: parsecs  Correlation between mass of the galactic distributions and their given blue luminosity (extracted from the Gravitational Wave Catalog reference) = correlation high = then, blue luminosity is a reasonable substitution for the mass of galactic distributions  Introducing basic constraints in relation to the potential number of SNe discovered using the Swift XRT technology  SN per century produced plot = rough estimation may be assumed by converting the mass into a SN estimation rate we assume: Rough estimation of 2 SNe per milky way unit mass per century would be discovered if around 3 SNe per galaxy was discovered  Theorized larger portion of SNe that will be found in the x-ray region using the XRT portion of the Swift Satellite due to the efficient transmission of X-rays.  Curve of galactic distributions within 20 Mpc; maps out Milky Way > Andromeda Clusterings > Virgo SuperCluster  Slope of the curve produced optically produces a cubic relationship nearing the 20 Mpc cutoff distance Centaurus A Whirlpool Galaxy Virgo Super Cluster Sombrero Galaxy Andromeda Galaxy Milky Way Galaxy Centaurus A