Lacaille’S Catalogue of Southern Deep-Sky Objects
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Arxiv:2012.09981V1 [Astro-Ph.SR] 17 Dec 2020 2 O
Contrib. Astron. Obs. Skalnat´ePleso XX, 1 { 20, (2020) DOI: to be assigned later Flare stars in nearby Galactic open clusters based on TESS data Olga Maryeva1;2, Kamil Bicz3, Caiyun Xia4, Martina Baratella5, Patrik Cechvalaˇ 6 and Krisztian Vida7 1 Astronomical Institute of the Czech Academy of Sciences 251 65 Ondˇrejov,The Czech Republic(E-mail: [email protected]) 2 Lomonosov Moscow State University, Sternberg Astronomical Institute, Universitetsky pr. 13, 119234, Moscow, Russia 3 Astronomical Institute, University of Wroc law, Kopernika 11, 51-622 Wroc law, Poland 4 Department of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University, Kotl´aˇrsk´a2, 611 37 Brno, Czech Republic 5 Dipartimento di Fisica e Astronomia Galileo Galilei, Vicolo Osservatorio 3, 35122, Padova, Italy, (E-mail: [email protected]) 6 Department of Astronomy, Physics of the Earth and Meteorology, Faculty of Mathematics, Physics and Informatics, Comenius University in Bratislava, Mlynsk´adolina F-2, 842 48 Bratislava, Slovakia 7 Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, H-1121 Budapest, Konkoly Thege Mikl´os´ut15-17, Hungary Received: September ??, 2020; Accepted: ????????? ??, 2020 Abstract. The study is devoted to search for flare stars among confirmed members of Galactic open clusters using high-cadence photometry from TESS mission. We analyzed 957 high-cadence light curves of members from 136 open clusters. As a result, 56 flare stars were found, among them 8 hot B-A type ob- jects. Of all flares, 63 % were detected in sample of cool stars (Teff < 5000 K), and 29 % { in stars of spectral type G, while 23 % in K-type stars and ap- proximately 34% of all detected flares are in M-type stars. -
Spring Fever Strikes
The MARCH 2002 DENVER OBSERVER Newsletter of the Denver Astronomical Society One Mile Nearer the Stars How Many in One Night?? Gearing up for the Messier Marathon? Those folks who are new to astronomy may not yet be able to relate to the sheer joy of braving the early-spring temperatures (brrrrr) for a full night (and morning—I’m talking dusk to dawn, here) of observing some of the most beautiful objects in the heavens. Why now? Because for only a few weeks during the year is it possible to see all of the Messier objects in one night. Astronomers will dig in their heels and tripods, get out the star charts (See Page 7), and knock off one object after the next. Some people actually catalog 70 of the available 110 targets and submit their achievements to the Astronomical League for the coveted Messier Certificate. Others just like to look at the beautiful celestial wonders like the one in the photo to the left. Either way, get out to the The Pleaides (M45) DSS on the weekend of the 15th and enjoy Image © Joe Gafford, 2002 the views!—PK Spring Fever Strikes President’s Corner .......... 2 MARCH SKIES 2002 f you’ve been reading your astronomy magazines, you know that by month’s Schedule of Events ......... 2 Iend, four naked-eye planets will grace the night skies. Jupiter is the main show-stopper but Saturn, Mars, and finally Venus will sparkle for all, moon or no moon. Remember that a Officers ......................... 2 little high-cloud haze can be good for telescopic planet observations. -
02 Southern Cross
Asterism Southern Cross The Southern Cross is located in the constellation Crux, the smallest of the 88 constellations. It is one of the most distinctive. With the four stars Mimosa BeCrux, Ga Crux, A Crux and Delta Crucis, forming the arms of the cross. The Southern Cross was also used as a remarkably accurate timepiece by all the people of the southern hemisphere, referred to as the ‘Southern Celestial Clock’ by the portuguese naturalist Cristoval D’Acosta. It is perpendicular as it passes the meridian, and the exact time can thus be calculated visually from its angle. The german explorer Baron Alexander von Humboldt, sailing across the southern oceans in 1799, wrote: “It is a timepiece, which advances very regularly nearly 4 minutes a day, and no other group of stars affords to the naked eye an observation of time so easily made”. Asterism - An asterism is a distinctive pattern of stars or a distinctive group of stars in the sky. Constellation - A grouping of stars that make an imaginary picture in the sky. There are 88 constellations. The stars and objects nearby The Main-Themes in asterism Southern Cross Southern Cross Ga Crux A Crux Mimosa, Be Crux Delta Crucis The Motives in asterism Southern Cross Crucis A Bayer / Flamsteed indication AM Arp+Madore - A Catalogue of Southern peculiar Galaxies and Associations [B10] Boss, 1910 - Preliminary General Catalogue of 6188 Stars C Cluster CCDM Catalogue des composantes d’étoiles doubles et multiples CD Cordoba Durchmusterung Declination Cel Celescope Catalog of ultraviolet Magnitudes CPC -
Arxiv:0804.4630V1 [Astro-Ph] 29 Apr 2008 I Ehnv20;Ficao 06) Ti Nti Oeas Role This in Is It 2006A)
DRAFT VERSION NOVEMBER 9, 2018 Preprint typeset using LATEX style emulateapj v. 05/04/06 OPEN CLUSTERS AS GALACTIC DISK TRACERS: I. PROJECT MOTIVATION, CLUSTER MEMBERSHIP AND BULK THREE-DIMENSIONAL KINEMATICS PETER M. FRINCHABOY1,2,3 AND STEVEN R. MAJEWSKI2 Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325, USA Draft version November 9, 2018 ABSTRACT We have begun a survey of the chemical and dynamical properties of the Milky Way disk as traced by open star clusters. In this first contribution, the general goals of our survey are outlined and the strengths and limita- tions of using star clusters as a Galactic disk tracer sample are discussed. We also present medium resolution (R 15,0000) spectroscopy of open cluster stars obtained with the Hydra multi-object spectrographs on the Cerro∼ Tololo Inter-American Observatory 4-m and WIYN 3.5-m telescopes. Here we use these data to deter- mine the radial velocities of 3436 stars in the fields of open clusters within about 3 kpc, with specific attention to stars having proper motions in the Tycho-2 catalog. Additional radial velocity members (without Tycho-2 proper motions) that can be used for future studies of these clusters were also identified. The radial velocities, proper motions, and the angular distance of the stars from cluster center are used to derive cluster member- ship probabilities for stars in each cluster field using a non-parametric approach, and the cluster members so-identified are used, in turn, to derive the reliable bulk three-dimensional motion for 66 of 71 targeted open clusters. -
First Scientific Results with the VLT in Visitor and Service Modes
No. 98 – December 1999 First Scientific Results with the VLT in Visitor and Service Modes Starting with this issue, The Messenger will regularly include scientific results obtained with the VLT. One of the results reported in this issue is a study of NGC 3603, the most massive visible H II region in the Galaxy, with VLT/ISAAC in the near-infrared Js, H, and Ks-bands and HST/WFPC2 at Hα and [N II] wavelengths. These VLT observations are the most sensitive near-infrared observations made to date of a dense starburst region, allowing one to in- vestigate with unprecedented quality its low-mass stellar population. The sensitivity limit to stars detected in all three bands corresponds to 0.1 M0 for a pre-main-sequence star of age 0.7 Myr. The observations clearly show that sub-solar-mass stars down to at least 0.1 M0 do form in massive starbursts (from B. Brandl, W. Brandner, E.K. Grebel and H. Zinnecker, page 46). Js versus Js–Ks colour-magnitude diagrams of NGC 3603. The left-hand panel contains all stars detected in all three wave- bands in the entire field of view (3.4′×3.4′, or 6 pc × 6 pc); the centre panel shows the field stars at r > 75″ (2.25 pc) around the cluster, and the right-hand panel shows the cluster population within r < 33″ (1pc) with the field stars statistically subtracted. The dashed horizontal line (left-hand panel) indicates the detection limit of the previous most sensitive NIR study (Eisenhauer et al. -
The History of Star Formation in the Galactic Young Open Cluster NGC 6231
Triggered Star Formation in a Turbulent ISM Proceedings IAU Symposium No. 237, 2006 c 2007 International Astronomical Union B. G. Elmegreen & J. Palouˇs, eds. doi:10.1017/S1743921307002736 The history of star formation in the Galactic young open cluster NGC 6231 Mario E. van den Ancker1 1European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany e-mail: [email protected] Abstract. We study the star formation history of the galactic young open cluster NGC 6231 using new, deep, wide-field BV RI imaging. Contrary to previous suggestions, we do not find a lack of low-mass cluster members; our derived mass function is compatible with a Salpeter IMF. The star formation history of NGC 6231 appears to be bi-modal, with a first wave of star formation activity 3–5 Myr ago, followed by a new generation of stars forming ∼ 1 Myr ago. Keywords. Star Formation, Pre-main sequence Stars, Open clusters and associations The star formation history of the rich open cluster NGC 6231 has been hotly debated in the literature ever since the suggestion by Eggen (1976) that a violent process must have triggered star formation in the region. In the largest photometric study of the region to date, Sung et al. (1998) suggested an abrupt decrease in the number of low-mass stars in NGC 6231 - giving further credibility to a scenario in which star formation in this region may have been triggered. Interestingly, Reed & Cudworth (2003), recently found that the trajectory of the globular cluster NGC 6397 intersected that of the natal cloud of NGC 6231 around five million years ago - close to the estimated age of NGC 6231 – thus providing a plausible candidate for the triggering mechanism. -
Publications of the Astronomical Society of the Pacific 106: 404-412, 1994 April
Publications of the Astronomical Society of the Pacific 106: 404-412, 1994 April CCD Photometry of the Galactic Globular Cluster NGC 6535 in the Β and Passbands Ata Sarajedini1 Kitt Peak National Observatory, National Optical Astronomy Observatories,2 P.O. Box 26732, Tucson, Arizona 85726-6732 Electronic mail: [email protected] Received 1993 October 15; accepted 1994 February 1 ABSTRACT. The first CCD color-magnitude diagram (CMD) in Β and V is presented for the Galactic globular cluster NGC 6535. From this CMD, which extends below the main-sequence turnoff, we draw the following conclusions: (1) The horizontal branch (HB) is predominantly blue in nature with no RR Lyrae variables known to be cluster members. Nonetheless, based on a comparison with clusters which have blue HBs and RR Lyraes (Ml5 and M79), we infer a mean HB magnitude of <^RR> = 15.73 ±0.11 for NGC 6535. (2) Again, via a direct comparison with the blue HBs of M15 and M79, we derive a cluster reddening oíE{B—V) =0.44±0.02. (3) When combined with the apparent color of the red-giant branch at the level of the HB, (B—V)g= 1.18 ±0.02, the derived reddening yields a metal abundance of [Fe/H] = —1.85 ±0.10, similar to that of NGC 6397. (4) Application of the AFT0_hb and Δ(5— F)SGB_To cluster dating techniques reveals no perceptible age difference between NGC 6535 and NGC 6397. (5) A significant population of nine blue-straggler candidates is detected in NGC 6535. However, this is too few to facilitate a meaningful analysis of their radial distribution. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Balog 2016 Apj 832 87.Pdf
PROTOPLANETARY AND TRANSITIONAL DISKS IN THE OPEN STELLAR CLUSTER IC 2395 Item Type Article Authors Balog, Zoltan; Siegler, Nick; Rieke, George H.; Kiss, L. L.; Muzerolle, James; Gutermuth, Robert A.; Bell, Cameron P. M.; Vinkó, J.; Su, Kate Y. L.; Young, E. T.; Gáspár, András Citation PROTOPLANETARY AND TRANSITIONAL DISKS IN THE OPEN STELLAR CLUSTER IC 2395 2016, 832 (1):87 The Astrophysical Journal DOI 10.3847/0004-637X/832/1/87 Publisher IOP PUBLISHING LTD Journal The Astrophysical Journal Rights © 2016. The American Astronomical Society. All rights reserved. Download date 29/09/2021 21:43:54 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/622451 The Astrophysical Journal, 832:87 (17pp), 2016 November 20 doi:10.3847/0004-637X/832/1/87 © 2016. The American Astronomical Society. All rights reserved. PROTOPLANETARY AND TRANSITIONAL DISKS IN THE OPEN STELLAR CLUSTER IC 2395 Zoltan Balog1, Nick Siegler2, G. H. Rieke3, L. L. Kiss4, James Muzerolle5, R. A. Gutermuth6, Cameron P. M. Bell7, J. VinkÓ8,K.Y.L.Su3, E. T. Young9, and András Gáspár3 1 Max Planck Institute for Astronomy, Heidelberg, D-69117, Germany; [email protected] 2 NASA Exoplanet Exploration Program, Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA 3 Steward Observatory, 933 N. Cherry Ave, University of Arizona, Tucson, AZ 85721, USA 4 Konkoly Observatory, Research Center for Astronomy and Earth Sciences, P.O. Box 67, H-1525 Budapest, Hungary 5 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 6 Department of Astronomy, University of Massachusetts, Amherst, MA, USA 7 Institute for Astronomy, ETH Zürich, Wolfgang-Pauli-Strasse 27, 8093, Zürich, Switzerland 8 Dept. -
Observing List Evening of 2011 Dec 25 at Boyden Observatory
Southern Skies Binocular list Observing List Evening of 2011 Dec 25 at Boyden Observatory Sunset 19:20, Twilight ends 20:49, Twilight begins 03:40, Sunrise 05:09, Moon rise 06:47, Moon set 20:00 Completely dark from 20:49 to 03:40. New Moon. All times local (GMT+2). Listing All Classes visible above 2 air mass and in complete darkness after 20:49 and before 03:40. Cls Primary ID Alternate ID Con Mag Size Distance RA 2000 Dec 2000 Begin Optimum End S.A. Ur. 2 PSA Difficulty Optimum EP Open Collinder 227 Melotte 101 Car 8.4 15.0' 6500 ly 10h42m12.0s -65°06'00" 01:32 03:31 03:54 25 210 40 challenging Glob NGC 2808 Car 6.2 14.0' 26000 ly 09h12m03.0s -64°51'48" 21:57 03:08 04:05 25 210 40 detectable Open IC 2602 Collinder 229 Car 1.6 100.0' 520 ly 10h42m58.0s -64°24'00" 23:20 03:31 04:07 25 210 40 obvious Open Collinder 246 Melotte 105 Car 9.4 5.0' 7200 ly 11h19m42.0s -63°29'00" 01:44 03:33 03:57 25 209 40 challenging Open IC 2714 Collinder 245 Car 8.2 14.0' 4000 ly 11h17m27.0s -62°44'00" 01:32 03:33 03:57 25 209 40 challenging Open NGC 2516 Collinder 172 Car 3.3 30.0' 1300 ly 07h58m04.0s -60°45'12" 20:38 01:56 04:10 24 200 30 obvious Open NGC 3114 Collinder 215 Car 4.5 35.0' 3000 ly 10h02m36.0s -60°07'12" 22:43 03:27 04:07 25 199 40 easy Neb NGC 3372 Eta Carinae Nebula Car 3.0 120.0' 10h45m06.0s -59°52'00" 23:26 03:32 04:07 25 199 38 easy Open NGC 3532 Collinder 238 Car 3.4 50.0' 1600 ly 11h05m39.0s -58°45'12" 23:47 03:33 04:08 25 198 38 easy Open NGC 3293 Collinder 224 Car 6.2 6.0' 7600 ly 10h35m51.0s -58°13'48" 23:18 03:32 04:08 25 199 -
August 2012 of You Know I Went to the Astronomical League Conference (Alcon) in Chicago at the Beginning of July with My Grandmother
BACKBACK BAYBAY observerobserver The Official Newsletter of the Back Bay Amateur Astronomers P.O. Box 9877, Virginia Beach, VA 23450-9877 Looking Up! Hello again! This month I actually have a story EPHEMERALS to tell, instead of just random ramblings. As most august 2012 of you know I went to the Astronomical League Conference (ALCon) in Chicago at the beginning of July with my grandmother. It was great. Not quite 08/24, 7:00 pm as good as last year, seeing as I had to pay for it Night Hike and they didn’t give me a check and a plaque this Northwest River Park year (last year I won the Horkheimer Youth award, which paid for my trip), but it was still a lot of fun, and very educational. I met a lot of cool 08/24, 8:00 pm people and definitely learned something. The Garden Stars whole trip was a big story, but a few events stand Norfolk Botanical Gardens out the most in my memory, and they’re all connected to some extent. 08/28, 7:00 pm Boardwalk Astronomy It all started on the day we got there. ALCon is Near 24th St Stage an annual four day conference usually in the VA Beach Oceanfront beginning of July. This year, the day we got there was July fourth. After checking in, taking a nap and 09/06, 7:30 pm dining, we decided to participate in the observing BBAA Monthly Meeting event outside the hotel. It was in a parking lot with lights, and fireworks, but there was a large moon TCC Campus and Saturn was up, so we went for it. -
Star Clusters
Star Clusters Culpeper Astronomy Club (CAC) Meeting May 21, 2018 Overview • Introductions • Main Topic: Star Clusters - Open and Globular • Constellations: Bootes, Canes Venatici, Coma Berenices • Observing Session - TBD Observing Session – 29 April 18 • Kicked off at about 6:30 p.m • Ended at about 1:30 a.m • Set up several telescopes • Three refractor’s (RAS -7”, f/12) • 11” CPC 1100 SCT (Dennis) • 12” Meade SCT • Targets included: • Venus • Moon • Several double stars • Several deep sky objects • Jupiter • Checked out Saturn and Mars at after arriving home – 2:30 a.m. Loaner Telescopes Jupiter near Opposition • Taken on 13 May 2018 by Jerry Sykes (Opposition 8 May) • Taken with a 120mm refractor, 3x barlow and ASI224mc video camera • First time using his ASI224mc camera • Took several videos through breaks in the clouds • Shot 21,700 frames in a little over two minutes. • Used 29% of 21,700 frames • Captured using Sharpcap • Stacked in AS!3 • Processed in Registax6 Stellar Evolution - The Birth • Stars are born within the clouds of dust and gas scattered throughout most galaxies (Orion Nebula) • Swirling cloud gives rise to knots with sufficient mass that the gas and dust can begin to collapse under its own gravitational attraction • As cloud collapses, material at the center heats up and begins gathering dust and gas (Protostar) • Spinning clouds may break up into two or three blobs resulting in paired or groups of multiple stars • Not all of this material ends up as part of a star — the remaining dust can become planets, asteroids,