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Unknown Amorphous Carbon II. LRS SPECTRA the Sample Consists Of
Table I A summary of the spectral -features observed in the LRS spectra of the three groups o-f carbon stars. The de-finition o-f the groups is given in the text. wavelength Xmax identification Group I B - 12 urn E1 9.7 M™ Silicate 12 - 23 jim E IB ^m Silicate Group II < 8.5 M"i A C2H2 CS? 12 - 16 f-i/n A 13.7 - 14 Mm C2H2 HCN? 8 - 10 Mm E 8.6 M"i Unknown 10 - 13 Mm E 11.3 - 11 .7 M«> SiC Group III 10 - 13 MJn E 11.3 - 11 .7 tun SiC B - 23 Htn C Amorphous carbon 1 The letter in this column indicates the nature o-f the -feature: A = absorption; E = emission; C indicates the presence of continuum opacity. II. LRS SPECTRA The sample consists of 304 carbon stars with entries in the LRS catalog (Papers I-III). The LRS spectra have been divided into three groups. Group I consists of nine stars with 9.7 and 18 tun silicate features in their LRS spectra pointing to oxygen-rich dust in the circumstellar shell. These sources are discussed in Paper I. The remaining stars all have spectra with carbon-rich dust features. Using NIR photometry we have shown that in the group II spectra the stellar photosphere is the dominant continuum. The NIR color temperature is of the order of 25OO K. Paper II contains a discussion of sources with this class of spectra. The continuum in the group III spectra is probably due to amorphous carbon dust. -
Kepler K2 Observations of the Intermediate Polar FO Aquarii 3
Mon. Not. R. Astron. Soc. 000, 1–8 () Printed 11 April 2016 (MN LATEX style file v2.2) Kepler K2 Observations of the Intermediate Polar FO Aquarii M. R. Kennedy1,2⋆, P. Garnavich2, E. Breedt3, T. R. Marsh3, B. T. G¨ansicke3, D. Steeghs3, P. Szkody4, Z. Dai5,6 1Department of Physics, University College Cork, Ireland. 2Department of Physics, University of Notre Dame, Notre Dame, IN 46556. 3Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK 4Department of Astronomy, University of Washington, Seattle, WA, USA 5Yunnan Observatories, Chinese Academy of Science, 650011, P. R. China 6Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, P. R. China 11 April 2016 ABSTRACT We present photometry of the intermediate polar FO Aquarii obtained as part of the K2 mission using the Kepler space telescope. The amplitude spectrum of the data confirms the orbital period of 4.8508(4) h, and the shape of the light curve is consistent with the outer edge of the accretion disk being eclipsed when folded on this period. The average flux of FO Aquarii changed during the observations, suggesting a change in the mass accretion rate. There is no evidence in the amplitude spectrum of a longer period that would suggest disk precession. The amplitude spectrum also shows the white dwarf spin period of 1254.3401(4) s, the beat period of 1351.329(2) s, and 31 other spin and orbital harmonics. The detected period is longer than the last reported period of 1254.284(16) s, suggesting that FO Aqr is now spinning down, and has a positive P˙ . -
NASA's Goddard Space Flight Center Laboratory for High Energy
1 NASA’s Goddard Space Flight Center Laboratory for High Energy Astrophysics Greenbelt, Maryland 20771 @S0002-7537~99!00301-7# This report covers the period from July 1, 1997 to June 30, Toshiaki Takeshima, Jane Turner, Ken Watanabe, Laura 1998. Whitlock, and Tahir Yaqoob. This Laboratory’s scientific research is directed toward The following investigators are University of Maryland experimental and theoretical research in the areas of X-ray, Scientists: Drs. Keith Arnaud, Manuel Bautista, Wan Chen, gamma-ray, and cosmic-ray astrophysics. The range of inter- Fred Finkbeiner, Keith Gendreau, Una Hwang, Michael Loe- ests of the scientists includes the Sun and the solar system, wenstein, Greg Madejski, F. Scott Porter, Ian Richardson, stellar objects, binary systems, neutron stars, black holes, the Caleb Scharf, Michael Stark, and Azita Valinia. interstellar medium, normal and active galaxies, galaxy clus- Visiting scientists from other institutions: Drs. Vadim ters, cosmic-ray particles, and the extragalactic background Arefiev ~IKI!, Hilary Cane ~U. Tasmania!, Peter Gonthier radiation. Scientists and engineers in the Laboratory also ~Hope College!, Thomas Hams ~U. Seigen!, Donald Kniffen serve the scientific community, including project support ~Hampden-Sydney College!, Benzion Kozlovsky ~U. Tel such as acting as project scientists and providing technical Aviv!, Richard Kroeger ~NRL!, Hideyo Kunieda ~Nagoya assistance to various space missions. Also at any one time, U.!, Eugene Loh ~U. Utah!, Masaki Mori ~Miyagi U.!, Rob- there are typically between twelve and eighteen graduate stu- ert Nemiroff ~Mich. Tech. U.!, Hagai Netzer ~U. Tel Aviv!, dents involved in Ph.D. research work in this Laboratory. Yasushi Ogasaka ~JSPS!, Lev Titarchuk ~George Mason U.!, Currently these are graduate students from Catholic U., Stan- Alan Tylka ~NRL!, Robert Warwick ~U. -
Society News Science News the Antikythera Mechanism Skinakas Observatory Spectroscopic Diagnostics of Galactic Nuclei Eclipsing Binaries
HIPPARCHOSHIPPARCHOS The Hellenic Astronomical Society Newsletter Volume 2, Issue 2 Society News Science News The Antikythera Mechanism Skinakas observatory Spectroscopic Diagnostics of Galactic Nuclei Eclipsing Binaries ISSN: 1790-9252 ʸ˱ˤ˳˶˱˹˯˩˭ˮˬ˰˱˙ ƋƜƠƦƓ6SHFLDO(GLWLRQ °ĆāąĆąõýĉýĊýĈØĉĊćąăąĂõ÷Ĉ çąÿąĈāóûÿĒĊÿý÷ĉĊćąăąĂõ÷ĆćóĆûÿă÷ûõă÷ÿĆûćõĆāąĀýØČôĉĊû Ċą 1H[6WDU 6( ă÷ ĉ÷Ĉ øąýþôĉûÿ ă÷ øćûõĊû čÿāÿòúûĈ ÷ĉĊóćûĈ Ćā÷ăôĊûĈù÷ā÷ĄõûĈĀ÷ÿòāā÷ĂûĊąĆòĊýĂ÷ûăĒĈĀąċĂĆÿąēÞ ăó÷ ąÿĀąùóăûÿ÷ 1H[6WDU 6( ĉċăúċòüûÿ ĆćďĊąČ÷ăô ûċčćýĉĊõ÷ Ăû ûĄûāÿùĂóăûĈ āûÿĊąċćùõûĈ Ā÷ÿ ÷ĆõĉĊûċĊą āĒùą ÷Ąõ÷Ĉ ĆćąĈ ĊÿĂô Ûûă Ćûćÿā÷ĂøòăûĊ÷ÿ ý Ćÿþ÷ăĒĊýĊ÷ ă÷ Ċą ĂûĊ÷ăÿĔĉûÿ ą ÷ùąć÷ĉĊôĈ ƌƞƢƜƨơƱƠƥ ăó÷ ąÿĀąùóăûÿ÷ 1H[6WDU 6( öÁ &HOHVWURQ ´¹ÅÀ«µ´¸ 1H[6WDU6( ĊýăĊûāûċĊ÷õ÷āóĄýĊýĈĊûčăąāąùõ÷ĈĒĆďĈĆāôćďĈ ÷ċĊąĂ÷ĊąĆąÿýĂóăą āûÿĊąċćùÿĀĒ ĉēĉĊýĂ÷ úċă÷ĊĒĊýĊ÷ ÷ă÷øòþĂÿĉýĈ Ăóĉď IODVK Ċąċ čûÿćÿĉĊýćõąċ ĊÿĈ ĀąćċČ÷õûĈ ãæäêÜâæ 1H[6WDU6( êëçæé 0DNVXWRY&DVVHJUDLQ¡¾»¿¾Ã¸¹Ë*R7R ûĆÿĉĊćĔĉûÿĈ 6WDU%ULJKW ;/7 Ċą ûĆ÷ă÷ĉĊ÷ĊÿĀĒ āąùÿĉĂÿĀĒ ÛàØãÜêèæéáØêæçêèæë PP l ûċþċùćòĂĂÿĉýĈĊąċĊýāûĉĀąĆõąċ6N\$OLJQpĀ÷ÿĆąāāòòāā÷ ÜéêØçæéêØéÞ PP ÜéêâæÚæé I £¢ ¢£¡¨¢¢ 6WDU%ULJKW;/7 ãûĊą1H[6WDU6(ûõĉĊûĉĊýþóĉýĊąċąúýùąēØĆāòûĆÿāóĄĊû ãÜÚïìÜâãÜÚÜßëäéÞ [ óă÷÷ăĊÿĀûõĂûăą÷ĆĒĊąĂûăąēĀ÷ÿĊąĊýāûĉĀĒĆÿąþ÷Ċąøćûÿùÿ÷ æèàØáæìØàäãÜÚÜßæé éêÞèàåÞ ØāĊ÷üÿĂąċþÿ÷Āô»´»¾Ã¬À ĉ÷ĈíćýĉÿùƹÿĔăĊ÷ĈĊýăĊûčăąāąùõ÷1H[6WDUĊ÷ĊýāûĉĀĒĆÿ÷ ¡¢¥ PP PP(/X[ 6( óčąċă Ċýă ÿĀ÷ăĒĊýĊ÷ ă÷ ûăĊąĆõĉąċă ĆûćõĆąċ ¡¤£¢ 6WDU3RLQWHU ÷ăĊÿĀûõĂûă÷ êą ĂĒăą Ćąċ óčûĊû ă÷ ĀòăûĊû ûõă÷ÿ ă÷ ĀąÿĊòĄûĊû £¡ ¢ 뺸¼¾Á ¨ PP »´kIOLSPLUURUl Ăóĉ÷÷ĆĒĊąĆćąĉąČþòāĂÿąĀ÷ÿă÷÷Ćąā÷ēĉûĊûĊąþó÷Ă÷ ÙØèæé NJ Ûûă ĄóćûĊû Ćąÿą ÷ăĊÿĀûõĂûăą ă÷ ûĆÿāóĄûĊû -
The X-Ray Universe 2017
The X-ray Universe 2017 6−9 June 2017 Centro Congressi Frentani Rome, Italy A conference organised by the European Space Agency XMM-Newton Science Operations Centre National Institute for Astrophysics, Italian Space Agency University Roma Tre, La Sapienza University ABSTRACT BOOK Oral Communications and Posters Edited by Simone Migliari, Jan-Uwe Ness Organising Committees Scientific Organising Committee M. Arnaud Commissariat ´al’´energie atomique Saclay, Gif sur Yvette, France D. Barret (chair) Institut de Recherche en Astrophysique et Plan´etologie, France G. Branduardi-Raymont Mullard Space Science Laboratory, Dorking, Surrey, United Kingdom L. Brenneman Smithsonian Astrophysical Observatory, Cambridge, USA M. Brusa Universit`adi Bologna, Italy M. Cappi Istituto Nazionale di Astrofisica, Bologna, Italy E. Churazov Max-Planck-Institut f¨urAstrophysik, Garching, Germany A. Decourchelle Commissariat ´al’´energie atomique Saclay, Gif sur Yvette, France N. Degenaar University of Amsterdam, the Netherlands A. Fabian University of Cambridge, United Kingdom F. Fiore Osservatorio Astronomico di Roma, Monteporzio Catone, Italy F. Harrison California Institute of Technology, Pasadena, USA M. Hernanz Institute of Space Sciences (CSIC-IEEC), Barcelona, Spain A. Hornschemeier Goddard Space Flight Center, Greenbelt, USA V. Karas Academy of Sciences, Prague, Czech Republic C. Kouveliotou George Washington University, Washington DC, USA G. Matt Universit`adegli Studi Roma Tre, Roma, Italy Y. Naz´e Universit´ede Li`ege, Belgium T. Ohashi Tokyo Metropolitan University, Japan I. Papadakis University of Crete, Heraklion, Greece J. Hjorth University of Copenhagen, Denmark K. Poppenhaeger Queen’s University Belfast, United Kingdom N. Rea Instituto de Ciencias del Espacio (CSIC-IEEC), Spain T. Reiprich Bonn University, Germany M. Salvato Max-Planck-Institut f¨urextraterrestrische Physik, Garching, Germany N. -
![The Occurrence and Architecture of Exoplanetary Systems Arxiv:1410.4199V1 [Astro-Ph.EP] 15 Oct 2014](https://docslib.b-cdn.net/cover/9298/the-occurrence-and-architecture-of-exoplanetary-systems-arxiv-1410-4199v1-astro-ph-ep-15-oct-2014-479298.webp)
The Occurrence and Architecture of Exoplanetary Systems Arxiv:1410.4199V1 [Astro-Ph.EP] 15 Oct 2014
Annu. Rev. Astron. Astrophys. 2015 The Occurrence and Architecture of Exoplanetary Systems Joshua N. Winn Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, Massachusetts, 02139-4307; [email protected] Daniel C. Fabrycky Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL, 60637; [email protected] Key Words exoplanets, extrasolar planets, orbital properties, planet formation Abstract The basic geometry of the Solar System|the shapes, spacings, and orientations of the planetary orbits|has long been a subject of fascination as well as inspiration for planet formation theories. For exoplanetary systems, those same properties have only recently come into focus. Here we review our current knowledge of the occurrence of planets around other stars, their orbital distances and eccentricities, the orbital spacings and mutual in- clinations in multiplanet systems, the orientation of the host star's rotation axis, and the properties of planets in binary-star systems. 1 INTRODUCTION Over the centuries, astronomers gradually became aware of the following properties of the Solar System: • The Sun has eight planets, with the four smaller planets (Rp = 0:4{1.0 R⊕) interior arXiv:1410.4199v1 [astro-ph.EP] 15 Oct 2014 to the four larger planets (3.9{11.2 R⊕). • The orbits are all nearly circular, with a mean eccentricity of 0.06 and individual eccentricities ranging from 0.0068{0.21. • The orbits are nearly aligned, with a root-mean-squared inclination of 1◦: 9 relative to the plane defined by the total angular momentum of the Solar System (the \invariable plane"), and individual inclinations ranging from 0◦: 33{6◦: 3. -
The Planets for 1955 24 Eclipses, 1955 ------29 the Sky and Astronomical Phenomena Month by Month - - 30 Phenomena of Jupiter’S S a Te Llite S
THE OBSERVER’S HANDBOOK FOR 1955 PUBLISHED BY The Royal Astronomical Society of Canada C. A. C H A N T, E d ito r RUTH J. NORTHCOTT, A s s is t a n t E d ito r DAVID DUNLAP OBSERVATORY FORTY-SEVENTH YEAR OF PUBLICATION P r i c e 50 C e n t s TORONTO 13 Ross S t r e e t Printed for th e Society By the University of Toronto Press THE ROYAL ASTRONOMICAL SOCIETY OF CANADA The Society was incorporated in 1890 as The Astronomical and Physical Society of Toronto, assuming its present name in 1903. For many years the Toronto organization existed alone, but now the Society is national in extent, having active Centres in Montreal and Quebec, P.Q.; Ottawa, Toronto, Hamilton, London, and Windsor, Ontario; Winnipeg, Man.; Saskatoon, Sask.; Edmonton, Alta.; Vancouver and Victoria, B.C. As well as nearly 1000 members of these Canadian Centres, there are nearly 400 members not attached to any Centre, mostly resident in other nations, while some 200 additional institutions or persons are on the regular mailing list of our publications. The Society publishes a bi-monthly J o u r n a l and a yearly O b s e r v e r ’s H a n d b o o k . Single copies of the J o u r n a l are 50 cents, and of the H a n d b o o k , 50 cents. Membership is open to anyone interested in astronomy. Annual dues, $3.00; life membership, $40.00. -
Astrophysicists Discover Dimming of Binary Star 16 January 2017, by Brian Wallheimer
Astrophysicists discover dimming of binary star 16 January 2017, by Brian Wallheimer tell time. The star turned out to have other plans for the summer." Intermediate polars are interesting binary systems because the low-density star drops gas toward the compact dwarf, which catches the matter using its strong magnetic field and funnels it to the surface, a process called accretion. The gas emits X-rays and optical light as it falls, and we see regular light variations as the stars orbit and spin. Graduate student Mark Kennedy studied the light variations in detail during the three months the Kepler Space Telescope was pointing at FO Aquarii in 2014. Kennedy is a Naughton Fellow from University Sarah L. Krizmanich Telescope. Credit: University of College, Cork, in Ireland who spent a year and a Notre Dame half working at Notre Dame on interacting binary stars. "Kepler observed FO Aquarii every minute for three months, and Mark's analysis of the data made us think we knew all we could know about this star," A team of University of Notre Dame astrophysicists Garnavich said. led by Peter Garnavich, professor of physics, has observed the unexplained fading of an interacting Once Kepler was pointed in a new direction, binary star, one of the first discoveries using the Garnavich and his group used the Krizmanich University's Sarah L. Krizmanich Telescope. Telescope to continue the study. The binary star, FO Aquarii, located in the Milky "Just after the star came around the sun last year, Way galaxy and Aquarius constellation about 500 we started looking at it through the Krizmanich light-years from Earth, consists of a white dwarf Telescope, and we were shocked to see it was and a companion star donating gas to the compact seven times fainter than it had ever been before," dwarf, a type of binary system known as an said Colin Littlefield, a member of the Garnavich intermediate polar. -
A Review of the Disc Instability Model for Dwarf Novae, Soft X-Ray Transients and Related Objects a J.M
A review of the disc instability model for dwarf novae, soft X-ray transients and related objects a J.M. Hameury aObservatoire Astronomique de Strasbourg ARTICLEINFO ABSTRACT Keywords: I review the basics of the disc instability model (DIM) for dwarf novae and soft-X-ray transients Cataclysmic variable and its most recent developments, as well as the current limitations of the model, focusing on the Accretion discs dwarf nova case. Although the DIM uses the Shakura-Sunyaev prescription for angular momentum X-ray binaries transport, which we know now to be at best inaccurate, it is surprisingly efficient in reproducing the outbursts of dwarf novae and soft X-ray transients, provided that some ingredients, such as irradiation of the accretion disc and of the donor star, mass transfer variations, truncation of the inner disc, etc., are added to the basic model. As recently realized, taking into account the existence of winds and outflows and of the torque they exert on the accretion disc may significantly impact the model. I also discuss the origin of the superoutbursts that are probably due to a combination of variations of the mass transfer rate and of a tidal instability. I finally mention a number of unsolved problems and caveats, among which the most embarrassing one is the modelling of the low state. Despite significant progresses in the past few years both on our understanding of angular momentum transport, the DIM is still needed for understanding transient systems. 1. Introduction tems using Doppler tomography techniques (Steeghs et al. 1997; Marsh and Horne 1988; see also Marsh and Schwope Dwarf novae (DNe) are cataclysmic variables (CV) that 2016 for a recent review). -
Meeting Program
A A S MEETING PROGRAM 211TH MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY WITH THE HIGH ENERGY ASTROPHYSICS DIVISION (HEAD) AND THE HISTORICAL ASTRONOMY DIVISION (HAD) 7-11 JANUARY 2008 AUSTIN, TX All scientific session will be held at the: Austin Convention Center COUNCIL .......................... 2 500 East Cesar Chavez St. Austin, TX 78701 EXHIBITS ........................... 4 FURTHER IN GRATITUDE INFORMATION ............... 6 AAS Paper Sorters SCHEDULE ....................... 7 Rachel Akeson, David Bartlett, Elizabeth Barton, SUNDAY ........................17 Joan Centrella, Jun Cui, Susana Deustua, Tapasi Ghosh, Jennifer Grier, Joe Hahn, Hugh Harris, MONDAY .......................21 Chryssa Kouveliotou, John Martin, Kevin Marvel, Kristen Menou, Brian Patten, Robert Quimby, Chris Springob, Joe Tenn, Dirk Terrell, Dave TUESDAY .......................25 Thompson, Liese van Zee, and Amy Winebarger WEDNESDAY ................77 We would like to thank the THURSDAY ................. 143 following sponsors: FRIDAY ......................... 203 Elsevier Northrop Grumman SATURDAY .................. 241 Lockheed Martin The TABASGO Foundation AUTHOR INDEX ........ 242 AAS COUNCIL J. Craig Wheeler Univ. of Texas President (6/2006-6/2008) John P. Huchra Harvard-Smithsonian, President-Elect CfA (6/2007-6/2008) Paul Vanden Bout NRAO Vice-President (6/2005-6/2008) Robert W. O’Connell Univ. of Virginia Vice-President (6/2006-6/2009) Lee W. Hartman Univ. of Michigan Vice-President (6/2007-6/2010) John Graham CIW Secretary (6/2004-6/2010) OFFICERS Hervey (Peter) STScI Treasurer Stockman (6/2005-6/2008) Timothy F. Slater Univ. of Arizona Education Officer (6/2006-6/2009) Mike A’Hearn Univ. of Maryland Pub. Board Chair (6/2005-6/2008) Kevin Marvel AAS Executive Officer (6/2006-Present) Gary J. Ferland Univ. of Kentucky (6/2007-6/2008) Suzanne Hawley Univ. -
Arxiv:2001.10147V1
Magnetic fields in isolated and interacting white dwarfs Lilia Ferrario1 and Dayal Wickramasinghe2 Mathematical Sciences Institute, The Australian National University, Canberra, ACT 2601, Australia Adela Kawka3 International Centre for Radio Astronomy Research, Curtin University, Perth, WA 6102, Australia Abstract The magnetic white dwarfs (MWDs) are found either isolated or in inter- acting binaries. The isolated MWDs divide into two groups: a high field group (105 − 109 G) comprising some 13 ± 4% of all white dwarfs (WDs), and a low field group (B < 105 G) whose incidence is currently under investigation. The situation may be similar in magnetic binaries because the bright accretion discs in low field systems hide the photosphere of their WDs thus preventing the study of their magnetic fields’ strength and structure. Considerable research has been devoted to the vexed question on the origin of magnetic fields. One hypothesis is that WD magnetic fields are of fossil origin, that is, their progenitors are the magnetic main-sequence Ap/Bp stars and magnetic flux is conserved during their evolution. The other hypothesis is that magnetic fields arise from binary interaction, through differential rotation, during common envelope evolution. If the two stars merge the end product is a single high-field MWD. If close binaries survive and the primary develops a strong field, they may later evolve into the arXiv:2001.10147v1 [astro-ph.SR] 28 Jan 2020 magnetic cataclysmic variables (MCVs). The recently discovered population of hot, carbon-rich WDs exhibiting an incidence of magnetism of up to about 70% and a variability from a few minutes to a couple of days may support the [email protected] [email protected] [email protected] Preprint submitted to Journal of LATEX Templates January 29, 2020 merging binary hypothesis. -
Keith Horne: Refereed Publications Papers Submitted: 425. “A
Keith Horne: Refereed Publications Papers Submitted: 427. “The Lick AGN Monitoring Project 2016: Velocity-Resolved Hβ Lags in Luminous Seyfert Galaxies.” V.U, A.J.Barth, H.A.Vogler, H.Guo, T.Treu, et al. (202?). ApJ, submitted (01 Oct 2021). 426. “Multi-wavelength Optical and NIR Variability Analysis of the Blazar PKS 0027-426.” E.Guise, S.F.H¨onig, T.Almeyda, K.Horne M.Kishimoto, et al. (202?). (arXiv:2108.13386) 425. “A second planet transiting LTT 1445A and a determination of the masses of both worlds.” J.G.Winters, et al. (202?) ApJ, submitted (30 Jul 2021). (arXiv:2107.14737) 424. “A Different-Twin Pair of Sub-Neptunes orbiting TOI-1064 Discovered by TESS, Characterised by CHEOPS and HARPS” T.G.Wilson et al. (202?). ApJ, submitted (12 Jul 2021). 423. “The LHS 1678 System: Two Earth-Sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc” M.L.Silverstein, et al. (202?). AJ, submitted (24 Jun 2021). 422. “A temperate Earth-sized planet with strongly tidally-heated interior transiting the M8 dwarf LP 791-18.” M.Peterson, B.Benneke, et al. (202?). submitted (09 May 2021). 421. “The Sloan Digital Sky Survey Reverberation Mapping Project: UV-Optical Accretion Disk Measurements with Hubble Space Telescope.” Y.Homayouni, M.R.Sturm, J.R.Trump, K.Horne, C.J.Grier, Y.Shen, et al. (202?). ApJ submitted (06 May 2021). (arXiv:2105.02884) Papers in Press: 420. “Bayesian Analysis of Quasar Lightcurves with a Running Optimal Average: New Time Delay measurements of COSMOGRAIL Gravitationally Lensed Quasars.” F.R.Donnan, K.Horne, J.V.Hernandez Santisteban (202?) MNRAS, in press (28 Sep 2021).