The Astrophysical Journal, often abbreviated ApJ in references and speech, is a peer-reviewed scientific journal of astrophysics and astronomy, established in 1895 by American astronomers George Ellery Hale and James Edward Keeler. The journal discontinued its print edition and became an electronic-only journal in 2015.
The SAO/NASA Astrophysics Data System (ADS) is an online database of over 16 million astronomy and physics papers from both peer reviewed and non-peer reviewed sources. Abstracts are available free online for almost all articles, and full scanned articles are available in Graphics Interchange Format (GIF) and Portable Document Format (PDF) for older articles. It was developed by the National Aeronautics and Space Administration (NASA), and is managed by the Smithsonian Astrophysical Observatory.
Monthly Notices of the Royal Astronomical Society (MNRAS) is a peer-reviewed scientific journal covering research in astronomy and astrophysics. It has been in continuous existence since 1827 and publishes letters and papers reporting original research in relevant fields. Despite the name, the journal is no longer monthly, nor does it carry the notices of the Royal Astronomical Society.
The American Meteor Society, Ltd. (AMS) is a non-profit scientific organization established to encourage and support the research activities of both amateur and professional astronomers who are interested in the field of meteor astronomy. Its affiliates observe, monitor, collect data on, study, and report on meteors, meteor showers, meteoric fireballs, and related meteoric phenomena.
Eta Ursae Majoris, formally named Alkaid, is a star in the constellation of Ursa Major. It is the most eastern (leftmost) star in the Big Dipper asterism. However, unlike most stars of the Big Dipper, it is not a member of the Ursa Major moving group. With an apparent visual magnitude of +1.84, it is the third-brightest star in the constellation and one of the brightest stars in the night sky.
T Coronae Borealis, is a recurring nova in the constellation Corona Borealis. It was first discovered in outburst in 1866 by John Birmingham, although it had been observed earlier as a 10th magnitude star.
HD 1606 is a single star in the northern constellation of Andromeda, positioned a few degrees to the northeast of the bright star Alpheratz. It has a blue-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.87. Although it is suspected of variability, none has been conclusively found. The star is located at a distance of approximately 580 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +4 km/s. It has an absolute magnitude of −0.5.
Astronomy & Astrophysics is a peer-reviewed scientific journal covering theoretical, observational, and instrumental astronomy and astrophysics. The journal is run by a Board of Directors representing 27 sponsoring countries plus a representative of the European Southern Observatory. The main editors of A&A are the editor-in-chief, Thierry Forveille; the Letters editor-in-chief, João Alves; and the managing editor David Elbaz. The journal is published by EDP Sciences in 12 issues per year.
HAT-P-4 is a wide binary star consisting of a pair of G-type main-sequence stars in the constellation of Boötes. It is also designated BD+36°2593.
Ofer Lahav is Perren Chair of Astronomy at University College London (UCL), Vice-Dean (International) of the UCL Faculty of Mathematical and Physical Sciences (MAPS) and Co-Director of the STFC Centre for Doctoral Training in Data Intensive Science. His research area is Observational Cosmology, in particular probing Dark Matter and Dark Energy. His work involves Machine Learning for Big Data.
Astronomy & Geophysics (A&G) is a scientific journal and trade magazine published on behalf of the Royal Astronomical Society (RAS) by Oxford University Press. It publishes a mixture of content of interest to astronomers and geophysicists: news reports, interviews, topical reviews, historical investigations, obituaries, meeting reports and updates on the activities of the RAS. Full-length articles are peer reviewed.
S Muscae is a classical (δ) Cepheid variable star in the constellation Musca about 2,600 light years away.
W Cygni is a semi-regular variable star in the constellation Cygnus, located 570 light-years from Earth. It lies less than half a degree southeast of ρ Cygni. W Cygni is, at times, a naked-eye star but it was not given a Bayer or Flamsteed designation. It has been proposed as a binary star system with a hotter main sequence companion, but this has not been confirmed.
Q Cygni, is a star located in the constellation Cygnus. It is also known as Nova Cygni 1876, and has the designation NGC 7114, and HR 8296. Nova Cygni is located in the northwestern portion of Cygnus along the border with Lacerta.
William Pendry Bidelman was an American astronomer. Born in Los Angeles, and raised in North Dakota, he was noted for classifying the spectra of stars, and considered a pioneer in recognizing and classifying sub-groups of the peculiar stars.
HD 163840 is a binary star system in the northern constellation of Hercules. It has a combined apparent visual magnitude of 6.45, which falls just below the brightness level that is visible to the naked eye for people with normal eyesight. An annual parallax shift of 35.40 mas provides a distance estimate of about 92 light years. The system is moving closer to the Sun with a radial velocity of −33 km/s. In about 769,000 years, it will make perihelion at a separation of around 27.2 ly (8.33 pc).
HD 60803 is a binary star system in the equatorial constellation of Canis Minor, located less than a degree to the northwest of the prominent star Procyon. It has a yellow hue and is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.904. The distance to this system is 135 light years as determined using parallax measurements, and is drifting further away with a radial velocity of +4.6 km/s.
RS Canum Venaticorum is a binary star system in the northern constellation of Canes Venatici. It serves as the prototype to the class of RS Canum Venaticorum variables. The peak apparent visual magnitude of this system is below the level needed to observe it with the naked eye. It is located at a distance of approximately 443 light years from the Sun based on parallax, but is drifting closer with a net radial velocity of −14 km/s. Olin J. Eggen (1991) included this system as a member of the IC 2391 supercluster, but it was later excluded.
SZ Piscium is a suspected triple star system in the equatorial constellation of Pisces. The inner pair form a double-lined spectroscopic binary with an orbital period of 3.966 days. It is a detached Algol-type eclipsing binary of the RS Canum Venaticorum class with a subgiant component. The system is too faint to be readily visible to the naked eye with a combined apparent visual magnitude of 7.18. It is located at a distance of approximately 306 light years based on parallax measurements.
