1. ` Short-Term Variability in Quasar Magnitude Brian T. Fleming 1, Julia Kennefick 2, S. Bursick 2 1 Illinois Institute of Technology, Chicago, IL USA Sequential Logic 2 University of Arkansas, Fayetteville, AR USA Understanding Quazi-Stellar Objects (QSO’s) First observed in 50’s as radio sources without a corresponding visible source. 1960 - 3C 48 tied to faint blue star-like object – Spectrum contained anomalous emission lines. Classified as “unknown” 1963 – 3C 273 determined to have a redshift of z=0.1592 Traveling away from Earth at 44,000 km / sec Nearly 2 billion light years away (Using Hubble’s Law: ) Dubbed Quazi-Stellar Objects because they looked like stars Today it is known that quasars are galaxies with super-massive black holes – differentiated from the term “QSO” Only about 10% are radio sources (“Radio Loud Quasars”) Excited matter accelerated in the accretion disk of the black hole give off staggering amounts of energy (~1.8 x 10 46 ergs/s for 3C 273 ≈ 4.7 trillion suns) Most distant and luminous objects known Quasar Detection and Identification The NFO Webscope Robotic Telescope 24 Inch diameter Capable of resolving objects with m≤18 with stacked images Quasars usually appear as stars in optical wavelengths Too distant to resolve as galaxies with most telescopes Differentiated from stars using spectroscopy – most common method of detection Stars fall in highly populated color region (fig.1 – left 4 ) due to stellar cores being primarily dominant fusion cycles Quasars (and other anomalous objects) will usually outside the populous region Spectra of the Anomalous Objects that reveal strong emission lines for Hydrogen (primary element in a galaxy) identify objects as quasars (fig.2 – right 5 ) The QUEST Quasar Variability Survey 6 Quasars Selected for Variability Study Five known Quasars were selected using the NASA Extragalactic Database (NED) for this study Three areas of sky were observed using the NFO Webscope with two of those areas containing two separate quasars resolvable by the telescope In order to help find the quasar in each image, the quasar’s relationship to neighboring objects was established. In figures 3-5 below the quasar is marked by the purple circle. Fig. 3 HS 1603+3820 High magnitude and redshift Magnitude: 15.9 Redshift: 2.51 Fig. 4 VCV J162021.8+173623 Magnitude: 16.4 Redshift: z = 0.55510 VCV J162011.3+172428 Magnitude: 15.5 Redshift: z = 0.11244 Fig. 5 Previously studied for variability. QUEST J150724.0-020212.1 Magnitude: 14.5 Redshift: 1.090 QUEST J150706.7-020728.9 Magnitude: 17.3 Redshift: 1.920 Quasar Variability Type of matter in the accretion disk is not constant with time Galaxies, while primarily Hydrogen, are not uniform Supernova remnants will be rich in heavy elements Amount of matter is also not constant Larger and older galaxies tend to have pockets of heavier concentration of matter due to gravity Spiral galaxies have spaces between the arms Over time, these fluctuations will cause noticeable variation in the wavelength (and magnitude) of light emitted Purpose of Study Fig. 7 – A Quasar. The outer edge of the accretion disk is barely visible partially eclipsing the luminous region 6 Procedure Take Images as often as possible over study time period (45 days) Monitor change in nearby stable stars to remove interference Subtract average stellar variation from quasar variation Record day to day quasar magnitude variation Observe five (5) quasars for 45 daysObserve five (5) quasars for 45 days Can the QUEST quasar variation be detectedCan the QUEST quasar variation be detected Look for variation in the other quasars Look for variation in the other quasars ChallengesChallenges Short time intervalShort time interval Faint magnitudes push limits of the NFO webscopeFaint magnitudes push limits of the NFO webscope Will help set standard for quasar variability astronomy limitsWill help set standard for quasar variability astronomy limits Quasar Variability Observed Primary References 3 Quasar Astronomy Daniel W. Weedman, Cambridge University Press, 1986 4 University of Tokyo, “Multicolor Survey for High Redshift Quasars”, S. Oyabu, 1998 5 The Astrophysical Journal, “2DF QSO Redshift Survey”, S.M Croom, 1998 6 The Astrophysical Journal, “New Quasars Detected Via Variability in the QUEST1 Survey”, A.W Rengstorf, May 2004 QUEST survey concluded that with a 80% confidence level, about 75% of quasars that they surveyed will show variability over a 26 month period6 50% will show at least 0.15 mag variation over 2 years Nearly all will vary by at least 0.05 mag over 15 years The QUEST survey was the first survey to use variation as a means of quasar discovery as opposed to the standard multi-color analysis method Fig. 6 A plot of magnitude versus time for the QUEST J140621.6- 012121.2 quasar. 6 Fig 8 – Red Filter VCV J162011.3+172428 No appreciable variation. Slight downward trend within error range. 13 days observed. Fig 9 – Red Filter VCV J162021.8+173623 No appreciable variation. Slight upward trend within error range. 13 days observed. Fig 10 – Red Filter HS 1603+3820 No appreciable variation. 9 days observed