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Wide-Field Infrared Survey Explorer Observations of the Evolution of Massive Star-Forming Regions
The Astrophysical Journal, 744:130 (24pp), 2012 January 10 doi:10.1088/0004-637X/744/2/130 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. WIDE-FIELD INFRARED SURVEY EXPLORER OBSERVATIONS OF THE EVOLUTION OF MASSIVE STAR-FORMING REGIONS X. P. Koenig1,4,D.T.Leisawitz1, D. J. Benford1, L. M. Rebull2, D. L. Padgett1, and R. J. Assef3,4 1 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 2 Spitzer Science Center (SSC), California Institute of Technology, M/S 220-6, 1200 East California Boulevard, Pasadena, CA 91125, USA 3 Jet Propulsion Laboratory, MS 169-530, 4800 Oak Grove Drive, Pasadena, CA 91109, USA Received 2011 July 8; accepted 2011 October 18; published 2011 December 22 ABSTRACT We present the results of a mid-infrared survey of 11 outer Galaxy massive star-forming regions and 3 open clusters with data from the Wide-field Infrared Survey Explorer (WISE). Using a newly developed photometric scheme to identify young stellar objects and exclude extragalactic contamination, we have studied the distribution of young stars within each region. These data tend to support the hypothesis that latter generations may be triggered by the interaction of winds and radiation from the first burst of massive star formation with the molecular cloud material leftover from that earlier generation of stars. We dub this process the “fireworks hypothesis” since star formation by this mechanism would proceed rapidly and resemble a burst of fireworks. We have also analyzed small cutout WISE images of the structures around the edges of these massive star-forming regions. -
Calibrating the Fundamental Plane with SDSS DR8 Data⋆
A&A 557, A21 (2013) Astronomy DOI: 10.1051/0004-6361/201321466 & c ESO 2013 Astrophysics Calibrating the fundamental plane with SDSS DR8 data Christoph Saulder1,2,Steffen Mieske1, Werner W. Zeilinger2, and Igor Chilingarian3,4 1 European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago, Chile e-mail: [csaulder,smieske]@eso.org 2 Department of Astrophysics, University of Vienna, Türkenschanzstraße 17, 1180 Vienna, Austria e-mail: [email protected] 3 Smithsonian Astrophysical Observatory, Harvard-Smithsonian Center for Astrophysics, 60 Garden St. MS09 Cambridge, MA 02138, USA e-mail: [email protected] 4 Sternberg Astronomical Institute, Moscow State University, 13 Universitetski prospect, 119992 Moscow, Russia Received 13 March 2013 / Accepted 27 May 2013 ABSTRACT We present a calibration of the fundamental plane using SDSS Data Release 8. We analysed about 93 000 elliptical galaxies up to z < 0.2, the largest sample used for the calibration of the fundamental plane so far. We incorporated up-to-date K-corrections and used GalaxyZoo data to classify the galaxies in our sample. We derived independent fundamental plane fits in all five Sloan filters u, g, r, i,andz. A direct fit using a volume-weighted least-squares method was applied to obtain the coefficients of the fundamental plane, which implicitly corrects for the Malmquist bias. We achieved an accuracy of 15% for the fundamental plane as a distance indicator. We provide a detailed discussion on the calibrations and their influence on the resulting fits. These re-calibrated fundamental plane relations form a well-suited anchor for large-scale peculiar-velocity studies in the nearby universe. -
Astronomy Magazine Special Issue
γ ι ζ γ δ α κ β κ ε γ β ρ ε ζ υ α φ ψ ω χ α π χ φ γ ω ο ι δ κ α ξ υ λ τ μ β α σ θ ε β σ δ γ ψ λ ω σ η ν θ Aι must-have for all stargazers η δ μ NEW EDITION! ζ λ β ε η κ NGC 6664 NGC 6539 ε τ μ NGC 6712 α υ δ ζ M26 ν NGC 6649 ψ Struve 2325 ζ ξ ATLAS χ α NGC 6604 ξ ο ν ν SCUTUM M16 of the γ SERP β NGC 6605 γ V450 ξ η υ η NGC 6645 M17 φ θ M18 ζ ρ ρ1 π Barnard 92 ο χ σ M25 M24 STARS M23 ν β κ All-in-one introduction ALL NEW MAPS WITH: to the night sky 42,000 more stars (87,000 plotted down to magnitude 8.5) AND 150+ more deep-sky objects (more than 1,200 total) The Eagle Nebula (M16) combines a dark nebula and a star cluster. In 100+ this intense region of star formation, “pillars” form at the boundaries spectacular between hot and cold gas. You’ll find this object on Map 14, a celestial portion of which lies above. photos PLUS: How to observe star clusters, nebulae, and galaxies AS2-CV0610.indd 1 6/10/10 4:17 PM NEW EDITION! AtlAs Tour the night sky of the The staff of Astronomy magazine decided to This atlas presents produce its first star atlas in 2006. -
Southwest Florida Astronomical Society SWFAS
Southwest Florida Astronomical Society SWFAS The Eyepiece September 2013 A MESSAGE FROM THE PRESIDENT I hope everyone had a good Labor Day weekend! Well, as I said last month, Comet ISON is on its way. How it will perform is still uncertain. I will be talking about it and other upcoming events as our program this month. This summer the rain has really hurt observing. Did anyone get to see Nova Delphini at its brightest? We have a very busy fall/winter season with a lot of events and requests. Please let me know if you can help at any of the events. I will be sending out updated calendars regularly. Our October meeting program is to be determined. If you have a presentation or idea for a program, please let me know! Carole Holmberg has a public event planned for Friday Sept 13th at 8pm at the CNCP. The November meeting is our annual Telescope Renaissance night (with observing) starting at 7pm on the 7th at the CNCP. There will be no formal meeting that night. Moon: Sep New 5th, 1st Quarter 12th, Full 19th, Last Quarter 26th Oct New 4th, 1st Quarter 11th, Full 18th, Last Quarter 26th Star Parties: September 14, October 5, November 2, November 30, December 28. The planets: Venus is dominating the evening sky after sunset as Saturn slips further towards the sun. Mercury will make a brief appearance midmonth after sunset. Mars is reappearing in the morning sky (key to finding ISON) and Jupiter rises a few hours after midnight. Club Positions President: Program Coordinator: (239-940-2935) Brian Risley Vacant Club Historian: swfasbrisley@embarqmail. -
2014 Observers Challenge List
2014 TMSP Observer's Challenge Atlas page #s # Object Object Type Common Name RA, DEC Const Mag Mag.2 Size Sep. U2000 PSA 18h31m25s 1 IC 1287 Bright Nebula Scutum 20'.0 295 67 -10°47'45" 18h31m25s SAO 161569 Double Star 5.77 9.31 12.3” -10°47'45" Near center of IC 1287 18h33m28s NGC 6649 Open Cluster 8.9m Integrated 5' -10°24'10" Can be seen in 3/4d FOV with above. Brightest star is 13.2m. Approx 50 stars visible in Binos 18h28m 2 NGC 6633 Open Cluster Ophiuchus 4.6m integrated 27' 205 65 Visible in Binos and is about the size of a full Moon, brightest star is 7.6m +06°34' 17h46m18s 2x diameter of a full Moon. Try to view this cluster with your naked eye, binos, and a small scope. 3 IC 4665 Open Cluster Ophiuchus 4.2m Integrated 60' 203 65 +05º 43' Also check out “Tweedle-dee and Tweedle-dum to the east (IC 4756 and NGC 6633) A loose open cluster with a faint concentration of stars in a rich field, contains about 15-20 stars. 19h53m27s Brightest star is 9.8m, 5 stars 9-11m, remainder about 12-13m. This is a challenge obJect to 4 Harvard 20 Open Cluster Sagitta 7.7m integrated 6' 162 64 +18°19'12" improve your observation skills. Can you locate the miniature coathanger close by at 19h 37m 27s +19d? Constellation star Corona 5 Corona Borealis 55 Trace the 7 stars making up this constellation, observe and list the colors of each star asterism Borealis 15H 32' 55” Theta Corona Borealis Double Star 4.2m 6.6m .97” 55 Theta requires about 200x +31° 21' 32” The direction our Sun travels in our galaxy. -
Title Goes Here
Jurnal Fizik Malaysia Volume 39 Issue 1 (2018) pgs 10017-10028 Z. Zainal Abidin Study of A1367 Cluster by Curve Fitting Variations Zamri Zainal Abidina, Zainol Abidin Ibrahima, Low Wei Yewa, Muhammad Mustaqim Mezana, Danial Ahmad Ariffin Leea, and Christine Jordanb aRadio Cosmology Laboratory Department of Physics, Faculty of Science, University of Malaya, 50603 Kuala Lumpur, Malaysia. bThe School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL (Received: 17.12.2017 ; Published: 23.7.2018) Abstract. We investigate the possible gain spectrum of the A1367 cluster or more commonly known as the Leo cluster using different polynomial fitting techniques in DRAWSPEC. For one of the aspects of the research on the possible mass of dark matter in the Leo cluster, the mass of neutral hydrogen ( ) is to be determined using gain analysis in the DRAWSPEC programme, prior to using the virialized mass of the Leo cluster to determine the mass of dark matter in the cluster. This investigation is significant because by using different polynomial fittings, one set of data could yield different gain, thus providing different , ultimately affecting the calculation of mass of dark matter in a cluster. In this paper, we present a comparison between different gain spectrum and using different polynomial fittings and we conclude that the result yields different by using different curve fitting techniques. Keywords: galaxy cluster-curve fitting-neutral hydrogen mass-gain spectrum- DRAWSPEC I. INTRODUCTION When determining the mass of all the observable matter in a galaxy cluster, interstellar matter plays a role in contributing to the mass [1]. Among the interstellar matters taken into consideration, neutral hydrogen (HI) is chosen due to the fact that starlight is not required to give off 21cm line emission and is generally abundant in clusters [2]. -
Astronomy Club of Tulsa Observer August 2013
Astronomy Club of Tulsa Observer August 2013 Photo: The Night Sky from 3RF, by Jerry Mullenix. Thank you Jerry! Permission to reprint anything from this newsletter is granted, PROVIDED THAT CREDIT IS GIVEN TO THE ORIGINAL AUTHOR AND THAT THE ASTRONOMY CLUB OF TULSA “OBSERVER” IS LISTED AS THE ORIGINAL SOURCE. For original content credited to others and so noted in this publication, you should obtain permission from that respective source prior to re-printing. Thank you very much for your cooperation. Please enjoy this edition of the Observer. Inside This Edition: Article/Item Page Calendar and Upcoming Events 3 President’s Message, by Lee Bickle 4 Treasurer’s and Membership Report, by John Land 5 The Secretary’s Stuff, by Tamara Green 7 NITELOG, by Tom Hoffelder 10 Size Does Matter, But So Does Dark Energy, by Dr. Ethan Siegel 14 Where We Meet 17 Officers, Board, Staff and Membership Info 18 The Editor wishes a big fat To Owen Green, whose birthday is August 29! Many Happy Returns Owen! 2 August 2013 September 2013 Sun Mon Tue Wed Thu Fri Sat Sun Mon Tue Wed Thu Fri Sat 1 2 MN 3 MNB 1 2 3 4 5 6 MN 7 MNB 4 5 6 7 8 9 10 8 9 10 11 12 13 14 11 12 13 14 15 16 17 SW 15 16 17 18 19 20 CM 21 SW 18 19 20 21 22 23 PSP 24 22 23 24 25 26 27 28 PSPB PSPB 25 26 27 28 29 30 31 29 30 UPCOMING EVENTS: Sidewalk Astronomy Sat Aug 17 Bass Pro 7:45 PM Public Star Party Fri Aug 23 ACT Observatory 7:30 PM Labor Day Mon Sep 2 Members’ Night Fri Sep 6 ACT Observatory 7:00 PM General Meeting Fri Sep 20 TCC NE Campus 7:00 PM Sidewalk Astronomy Sat Sep 21 Bass Pro 7:15 PM Public Star Party Fri Sep 27 ACT Observatory 6:30 PM OKIE-TEX STAR PARTY is Sep 28 thru Oct 6 at Black Mesa! 3 President’s Message By Lee Bickle Hello everyone! Although July was a little unusual for us in the way of cooler temps and rain, we still had a busy month. -
A Mock Catalogue of Galaxy Luminosities, Colours and Positions for Cosmology
Durham E-Theses Rosella: A mock catalogue of galaxy luminosities, colours and positions for cosmology SAFONOVA, ALEKSANDRA How to cite: SAFONOVA, ALEKSANDRA (2019) Rosella: A mock catalogue of galaxy luminosities, colours and positions for cosmology, Durham theses, Durham University. Available at Durham E-Theses Online: http://etheses.dur.ac.uk/13321/ Use policy This work is licensed under a Creative Commons Attribution Non-commercial No Derivatives 2.0 UK: England & Wales (CC BY-NC-ND) Academic Support Oce, Durham University, University Oce, Old Elvet, Durham DH1 3HP e-mail: [email protected] Tel: +44 0191 334 6107 http://etheses.dur.ac.uk Rosella: A mock catalogue of galaxy luminosities, colours and positions for cosmology Sasha Safonova A thesis presented for the degree of Master of Science by Research Institute for Computational Cosmology Department of Physics The University of Durham United Kingdom August 2019 Dedicated to Margarita Safonova, who devoted her life to the search for controlled thermonuclear fusion and taught me that physics adds a game to any situation. Rosella: A mock catalogue of galaxy luminosities, colours and positions for cosmology Sasha Safonova Abstract The scientific exploitation of the Dark Energy Spectroscopic Instrument Bright Galaxy Survey (DESI BGS) data requires the construction of mocks with galaxy population properties closely mimicking those of the actual DESI BGS targets. We create a high fidelity mock galaxy catalogue that can be used to interpret the DESI BGS data, as well as meeting the precision required for the tuning of thousands of approximate DESI BGS mocks needed for cosmological analyses with DESI BGS data. -
Extended Ionized Gas out of Galaxies in the Leo Cluster (Abell 1367)
Extended Ionized Gas out of Galaxies in the Leo Cluster (Abell 1367) YAGI, Masafumi, YOSHIDA, Michitoshi, KOMIYAMA, Yutaka, KASHIKAWA, Nobunari (NAOJ) GAVAZZI, Giuseppe OKAMURA, Sadanori (University of Milano-Bicocca) (Hosei University) In clusters of galaxies, the relative motion of member galaxies to the hot gas of the cluster produces a ram pressure. The ram pressure strips gas from galaxies, and sometimes the gas stripped out of the galaxy gets ionized by some mechanism to be detected as an Hα emitting cloud. We observed a part of the Virgo cluster and the Coma cluster, in Hα narrow-band, and B, and R broad-bands of the Subaru Suprime-Cam to study such intergalactic ionized gas (e.g., [1,2]). We then executed a systematic survey of the Leo cluster (Abell 1367) with an Hα filter for redshift z=0.022 of the Suprime-Cam [3]. By the survey, we detected six new extended ionized gas clouds in addition to three galaxies with known gas tails (CGCG 097-073, CGCG 097-079, CGCG 097- 087; [4]), and one of the new clouds was confirmed to have much longer tail by a follow-up observation [5]. Remarkable objects compared to the previous studies were the clouds which show no relation to the galaxies; “Orphan clouds” (Figure 1 top). Other clouds known so far show the connection to the galaxy from which the gas came from (parent galaxies). Meanwhile, no parent candidates are found at least within 85 kpc from the orphan clouds, and any member galaxies around the region show no sign of stripping toward the orphans. -
8603517.PDF (12.42Mb)
Umversify Microfilins International 1.0 12.5 12.0 LI 1.8 1.25 1.4 1.6 MICROCOPY RESOLUTION TEST CHART NATIONAL BUREAU OF STANDARDS STANDARD REFERENCE MATERIAL 1010a (ANSI and ISO TEST CHART No. 2) University Microfilms Inc. 300 N. Zeeb Road, Ann Arbor, MI 48106 INFORMATION TO USERS This reproduction was made from a copy of a manuscript sent to us for publication and microfilming. While the most advanced technology has been used to pho tograph and reproduce this manuscript, the quality of the reproduction is heavily dependent upon the quality of the material submitted. Pages in any manuscript may have indistinct print. In all cases the best available copy has been filmed. The following explanation of techniques is provided to help clarify notations which may appear on this reproduction. 1. Manuscripts may not always be complete. When it is not possible to obtain missing pages, a note appears to indicate this. 2. When copyrighted materials are removed from the manuscript, a note ap pears to indicate this. 3. Oversize materials (maps, drawings, and charts) are photographed by sec tioning the original, beginning at the upper left hand comer and continu ing from left to right in equal sections with small overlaps. Each oversize page is also filmed as one exposure and is available, for an additional charge, as a standard 35mm slide or in black and white paper format.* 4. Most photographs reproduce acceptably on positive microfilm or micro fiche but lack clarify on xerographic copies made from the microfilm. For an additional charge, all photographs are available in black and white standard 35mm slide format. -
Arxiv:Astro-Ph/9906240V1 14 Jun 1999 Nteeouinr Ttso Estars Be Fabregat Juan of Status Evolutionary the on Orsodneto De- Correspondence to Is Issue Main the Question
A&A manuscript no. ASTRONOMY (will be inserted by hand later) AND Your thesaurus codes are: 05 (08.05.2; 08.05.3; 10.15.1) ASTROPHYSICS On the evolutionary status of Be stars Juan Fabregat1 and J. Miguel Torrej´on2 1 Departamento de Astronom´ıa, Universidad de Valencia, 46100 Burjassot, Valencia, Spain 2 Departamento de F´ısica, Ingenier´ıa de Sistemas y Teor´ıa de la Se˜nal, Universidad de Alicante, Spain Received date; accepted date Abstract. We present a study of the abundance of Be termine whether the Be phenomenon appears at a given stars in open clusters as a function of the cluster age, us- stage in the evolutionary track of every B star, or it orig- ing whenever possible ages determined through Str¨omgren inates in the conditions of formation of some stars, which uvby photometry. For the first time in studies of this kind include fast rotation and probably other facts. A funda- we have considered separately classical and Herbig Be mental element in this discussion is the study of Be stars stars. in open clusters, in two different ways: i./ the determina- The main results can be summarized as follows: tion of the Be star positions in the cluster photometric diagrams; and, ii./ the study of the abundance of Be stars – Clusters associated to emitting nebulosities and un- as a function of the cluster age. dergoing stellar formation are rich in emission line ob- It is well known that Be stars usually occupy anoma- jects, which most likely are all pre main-sequence stars. -
SAC's 110 Best of the NGC
SAC's 110 Best of the NGC by Paul Dickson Version: 1.4 | March 26, 1997 Copyright °c 1996, by Paul Dickson. All rights reserved If you purchased this book from Paul Dickson directly, please ignore this form. I already have most of this information. Why Should You Register This Book? Please register your copy of this book. I have done two book, SAC's 110 Best of the NGC and the Messier Logbook. In the works for late 1997 is a four volume set for the Herschel 400. q I am a beginner and I bought this book to get start with deep-sky observing. q I am an intermediate observer. I bought this book to observe these objects again. q I am an advance observer. I bought this book to add to my collect and/or re-observe these objects again. The book I'm registering is: q SAC's 110 Best of the NGC q Messier Logbook q I would like to purchase a copy of Herschel 400 book when it becomes available. Club Name: __________________________________________ Your Name: __________________________________________ Address: ____________________________________________ City: __________________ State: ____ Zip Code: _________ Mail this to: or E-mail it to: Paul Dickson 7714 N 36th Ave [email protected] Phoenix, AZ 85051-6401 After Observing the Messier Catalog, Try this Observing List: SAC's 110 Best of the NGC [email protected] http://www.seds.org/pub/info/newsletters/sacnews/html/sac.110.best.ngc.html SAC's 110 Best of the NGC is an observing list of some of the best objects after those in the Messier Catalog.