DOCSLIB.ORG

250 — 10 October 2013 Editor: Bo Reipurth ([email protected]) List of Contents

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

THE STAR FORMATION NEWSLETTER An electronic publication dedicated to early stellar/planetary evolution and molecular clouds No. 250 — 10 October 2013 Editor: Bo Reipurth ([email protected]) List of Contents The Star Formation Newsletter Interview ...................................... 3 My Favorite Object ............................ 5 Editor: Bo Reipurth [email protected] Perspective .................................... 9 Technical Editor: Eli Bressert Abstracts of Newly Accepted Papers .......... 13 [email protected] Abstracts of Newly Accepted Major Reviews . 51 Technical Assistant: Hsi-Wei Yen Dissertation Abstracts ........................ 52 [email protected] New Jobs ..................................... 54 Editorial Board Meetings ..................................... 57 Summary of Upcoming Meetings ............. 59 Joao Alves Alan Boss Short Announcements ........................ 60 Jerome Bouvier Lee Hartmann Thomas Henning Paul Ho Cover Picture Jes Jorgensen Charles J. Lada The image shows the reflection nebula NGC 7129 Thijs Kouwenhoven located in the Cepheus Flare at a distance of ap- Michael R. Meyer proximately 1250 pc and illuminated by three B- Ralph Pudritz stars. The Herbig Ae/Be star LkHα 234 is the Luis Felipe Rodr´ıguez bright nebulous star partly embedded in the cav- Ewine van Dishoeck ity rim (left of center). The main illuminators of Hans Zinnecker the reflection nebula are the two young B-stars BD+65◦1637 and BD+65◦1638 located inside the The Star Formation Newsletter is a vehicle for cavity (middle of figure). Numerous red Herbig- fast distribution of information of interest for as- Haro objects are seen, particularly the bright bow- tronomers working on star and planet formation shaped HH 103 (near the lower right edge). The and molecular clouds. You can submit material region is rich in low-mass pre-main sequence stars, for the following sections: Abstracts of recently radio continuum sources, and water masers. The B- accepted papers (only for papers sent to refereed stars have blown a cavity in a dense molecular cloud journals), Abstracts of recently accepted major re- about 11 pc in extent. Two molecular outflows are views (not standard conference contributions), Dis- associated with LkHα 234 and an embedded far- sertation Abstracts (presenting abstracts of new infrared source FIRS 2. Ph.D dissertations), Meetings (announcing meet- Image courtesy Johannes Schedler ings broadly of interest to the star and planet for- http://panther-observatory.com mation and early solar system community), New Jobs (advertising jobs specifically aimed towards persons within the areas of the Newsletter), and Short Announcements (where you can inform or re- quest information from the community). Addition- Submitting your abstracts ally, the Newsletter brings short overview articles on objects of special interest, physical processes or Latex macros for submitting abstracts theoretical results, the early solar system, as well and dissertation abstracts (by e-mail to as occasional interviews. [email protected]) are appended to each Call for Abstracts. You can also submit via the Newsletter Archive Newsletter web interface at http://www2.ifa. www.ifa.hawaii.edu/users/reipurth/newsletter.htm hawaii.edu/star-formation/index.cfm 2 46/47 outflow. What was the genesis of that paper? John Graham A: At that time, I was on the staff of Cerro Tololo Inter- American Observatory and Bok was coming to Chile on in conversation with Bo Reipurth observing visits. He had renewed his old interest in star formation within dark globules and had obtained a photo- graph of the HH46/47 outflow with the 4-meter telescope there. He was enthusiastic that others should follow up with spectroscopy and infrared photometry to identify the embedded source and to study the outflow. Q: Another very influential paper was your study with Jay Frogel on the new FUor associated with HH 57, and now known as V346 Nor. What is the story behind this discov- ery? A: Every researcher brings his or her own particular ex- pertise to the table. Mine was that I knew the southern skies unusually well and was very aware of any changes that might be taking place. I was familiar with the earlier work of Martin Cohen and Richard Schwartz in survey- Q: Your career started out in Australia where you studied ing areas of recent star formation and one night observing galactic structure. Was this motivated by Bart Bok, who HH 57 I noticed a star-like object that had not been there was the grand old man in that subject in those days? before, in the corner of the HH object. Subsequent com- A: It is important for all young scientists to have a men- munication with Schwartz confirmed that it had not been tor and I was lucky to come of age when Bart Bok had there when he last looked at it. just arrived in Australia as Director of the Mount Stromlo Q: You have documented how reflection nebulae around Observatory. Bart was an amazing character who com- some very young stars vary due to shadowing effects from bined great human warmth with a single-minded passion clouds moving around the stars, probably closer than 1 for his chosen science. Research into the structure of the AU. And you deduced spectroscopically that accretion onto Southern Milky Way was in its infancy at that time and it young stars is clumpy was a ripe field in which to get involved. My own doctoral A: This concerned the reflection nebula associated with research concerned using new distances for young O and the pre-main sequence star R CrA. Almost 100 years ago, early B type stars, some in clusters, some in the field, to Harold Knox-Shaw and Edwin Hubble had observed changes map Galactic spiral structure. in the morphology of the nebula taking place over several Q: Why did you move from Australia to The Netherlands? nights. Hubble correctly deduced that the phenomenon A: I went via South Africa. At the time of my graduation, was due to ’a wave of illumination’ sweeping across struc- the Leiden Observatory was unable to find an astronomer tures in the reflection nebula. I had the advantage of being to staff its southern observing station near Pretoria. The on the scientific staff of an observatory that provided ac- Director, Jan Oort, spoke to Bok, who suggested me as a cess to telescopes on sequential nights and could respond candidate. I took my PhD oral exam there at the Radcliffe to unexpected events at very short notice. Thanks to the Observatory from David Thackeray, who was another of newly available CCD detectors, I was able to image the R my mentors; a personality very different from Bok but CrA reflection nebula on several nights and could docu- who was a person equally passionate about his research. ment changes that could only be due to shadowing effects After a year in South Africa, I joined the staff at Leiden from partially opaque dust clouds very close to the star. but after a year was attracted to the Kitt Peak National The clumpy nature of the circumstellar material could Observatory by David Crawford, who was then in charge also be detected spectroscopically through night-to-night of building the 4-meter Mayall telescope. Kitt Peak was a changes in line intensities. Unfortunately, I was never able great place for a young astronomer in the 1960s because so to correlate the two phenomena. many renowned astronomers passed though there to use Q: Your most cited paper has nothing directly to do with the facilities. star formation, but deals with UBVRI standard stars in Q: You were among the pioneers in the early study of the E-regions. What motivated that study? Herbig-Haro objects and have published numerous papers A: I undertook that work because of the lack of faint pho- on the subject. I particularly remember your paper with tometric standard stars in the southern hemisphere and I Jay Elias from 1983 on the Bok globule harboring the HH needed them for my study of the Cepheid variable stars 3 in the southern galaxy NGC 300. That work led to my participation in the HST key project of using Cepheid variables to determine the distance scale and the Hub- ble constant. It was my one effort in large team research, otherwise I have always preferred to work in teams of two or three people. Q: In your most recent papers you moved to extragalactic star formation, studying young stars in Centaurus A and jets on a vastly larger scale. What were the main results? A: Those were two papers I wrote with Caleb Fassett in which we detailed the star formation that is triggered by the interaction of an extragalactic jet on an adjacent gas cloud. We were able to detect the ageing of the stars as they moved away from the regions of star formation and suggested that they would eventually contribute to the un- resolved, extended envelope of the radio galaxy. I believe that there is a lot more work to be done in examples such as this of star formation taking place under unusual cir- cumstances but I had more or less decided that it was time to stop active astronomical research and to get interested in other things. Towards the end of my scientific career, I took part in two service opportunities. For a year, I became a program officer in the Division of Astronomical Sciences at the Na- tional Science Foundation and, later on, for six years, was Secretary of the American Astronomical Society. While altruism played a part, I found a lot of satisfaction in see- ing for myself how things worked inside each of the two organizations, and I encourage those who can take the time to participate in community activities of this nature. Q: You have recently become interested in science educa- tion for high school students.
Recommended publications
  • Navigating North America

    Navigating North America

    deep-sky wonders by sue french Navigating North America the north america nebula is one of the most impres- NGC 6997 is the most obvious cluster within the confines sive nebulae glowing in our sky. This nebula’s remarkable of the North America Nebula. To me, it looks as though it’s resemblance to the North American continent makes it bet- been plunked down on the border between Ohio and West ter known by its common name — bestowed not by a resi- Virginia. Putting 4.8-magnitude 57 Cygni at the western dent of North America, but by German astrono- edge of a low-power eyepiece field should bring NGC 6997 Knowing mer Max Wolf. In 1890 Wolf became the first into view. My 4.1-inch scope at 17× displays a dusting of person to photograph the North America Nebula, very faint stars. At 47×, it’s a pretty cluster, rich in faint your and for many years this remained the only way to stars, spanning 10′. Through my 10-inch reflector, I count geography fully appreciate its distinctive shape. With today’s 40 stars, mostly of magnitude 11 and 12. Many are abundance of short-focal-length telescopes and arranged in two incomplete circles, one inside the other. puts you wide-field eyepieces, we can more readily enjoy Is NGC 6997 actually involved in the North America one step this large nebula visually. Nebula? It’s difficult to tell because the distances are poorly The North America Nebula, NGC 7000 or Cald- known. A journal article earlier this year puts NGC 6997 at ahead in well 20, is certainly easy to locate.
  • Arxiv:2012.09981V1 [Astro-Ph.SR] 17 Dec 2020 2 O

    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.
  • Filter Performance Comparisons for Some Common Nebulae

    Filter Performance Comparisons for Some Common Nebulae

    Filter Performance Comparisons For Some Common Nebulae By Dave Knisely Light Pollution and various “nebula” filters have been around since the late 1970’s, and amateurs have been using them ever since to bring out detail (and even some objects) which were difficult to impossible to see before in modest apertures. When I started using them in the early 1980’s, specific information about which filter might work on a given object (or even whether certain filters were useful at all) was often hard to come by. Even those accounts that were available often had incomplete or inaccurate information. Getting some observational experience with the Lumicon line of filters helped, but there were still some unanswered questions. I wondered how the various filters would rank on- average against each other for a large number of objects, and whether there was a “best overall” filter. In particular, I also wondered if the much-maligned H-Beta filter was useful on more objects than the two or three targets most often mentioned in publications. In the summer of 1999, I decided to begin some more comprehensive observations to try and answer these questions and determine how to best use these filters overall. I formulated a basic survey covering a moderate number of emission and planetary nebulae to obtain some statistics on filter performance to try to address the following questions: 1. How do the various filter types compare as to what (on average) they show on a given nebula? 2. Is there one overall “best” nebula filter which will work on the largest number of objects? 3.
  • NGC 1333 Plunkett Et

    NGC 1333 Plunkett Et

    Outflows in protostellar clusters: a multi-wavelength, multi-scale view Adele L. Plunkett1, H. G. Arce1, S. A. Corder2, M. M. Dunham1, D. Mardones3 1-Yale University; 2-ALMA; 3-Universidad de Chile Interferometer and Single Dish Overview Combination FCRAO-only v=-2 to 6 km/s FCRAO-only v=10 to 17 km/s K km s While protostellar outflows are generally understood as necessary components of isolated star formation, further observations are -1 needed to constrain parameters of outflows particularly within protostellar clusters. In protostellar clusters where most stars form, outflows impact the cluster environment by injecting momentum and energy into the cloud, dispersing the surrounding gas and feeding turbulent motions. Here we present several studies of very dense, active regions within low- to intermediate-mass Why: protostellar clusters. Our observations include interferometer (i.e. CARMA) and single dish (e.g. FCRAO, IRAM 30m, APEX) To recover flux over a range of spatial scales in the region observations, probing scales over several orders of magnitude. How: Based on these observations, we calculate the masses and kinematics of outflows in these regions, and provide constraints for Jy beam km s Joint deconvolution method (Stanimirovic 2002), CARMA-only v=-2 to 6 km/s CARMA-only v=10 to 17 km/s models of clustered star formation. These results are presented for NGC 1333 by Plunkett et al. (2013, ApJ accepted), and -1 comparisons among star-forming regions at different evolutionary stages are forthcoming. using the analysis package MIRIAD. -1 1212COCO Example: We mapped NGC 1333 using CARMA with a resolution of ~5’’ (or 0.006 pc, 1000 AU) in order to Our study focuses on Class 0 & I outflow-driving protostars found in clusters, and we seek to detect outflows and associate them with their driving sources.
  • A Campus Observatory Image of the North America Nebula

    A Campus Observatory Image of the North America Nebula

    The Observer A Campus Observatory Image of the North America Nebula by Fred Ringwald Fresno State’s Campus Observatory is convenient for students to use, but its sky rates 10 on the Bortle scale: “Most people don’t look up.” The faintest stars the unaided eye can see there are about 3rd magnitude. Nevertheless, its telescopes can get good images through an Hα (pronounced “H-alpha”) filter. An Hα filter passes only a narrow band of wavelengths that are centered on the Hα line, the scarlet wavelength at which hydrogen radiates the most light visible to the eye. City lights radiate mostly at other wavelengths, from mercury or sodium vapor in the lamps. Hydrogen is the most common element in nebulae, so Hα filters improve their image contrast. This image was taken through a 70-mm guidescope mounted piggyback on the Campus Observatory’s main telescope. The guidescope was made by Vixen. With a focal length of only 400 mm, the guidescope gets a wide field of view, which makes it easier for novice students to point the telescope. With the SBIG ST-9 camera used to take this image, the field of view is 1.5º on a side. It shows the southern end of NGC 7000, called “the North America Nebula” because of its shape. At upper right is “Florida,” bounded by a dust lane corresponding to the “Gulf of Mexico”; at bottom-center is “Mexico.” A bright shock front runs through the east side (on the left), which is called “the Great Wall,” incongruous since that’s in China! The North America Nebula is in the constellation Cygnus, 3º east of the 1st-magntude supergiant star Deneb.
  • Arxiv:2005.05466V1 [Astro-Ph.GA] 11 May 2020 Surface Density

    Arxiv:2005.05466V1 [Astro-Ph.GA] 11 May 2020 Surface Density

    Draft version May 13, 2020 Typeset using LATEX preprint style in AASTeX62 Star-Gas Surface Density Correlations in Twelve Nearby Molecular Clouds I: Data Collection and Star-Sampled Analysis Riwaj Pokhrel,1, 2 Robert A. Gutermuth,2 Sarah K. Betti,2 Stella S. R. Offner,3 Philip C. Myers,4 S. Thomas Megeath,1 Alyssa D. Sokol,2 Babar Ali,5 Lori Allen,6 Tom S. Allen,7, 8 Michael M. Dunham,9 William J. Fischer,10 Thomas Henning,11 Mark Heyer,2 Joseph L. Hora,4 Judith L. Pipher,12 John J. Tobin,13 and Scott J. Wolk4 1Ritter Astrophysical Research Center, Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606, USA 2Department of Astronomy, University of Massachusetts, 710 North Pleasant Street, Amherst, MA 01003, USA 3Department of Astronomy, The University of Texas at Austin, 2500 Speedway, Austin, TX 78712, USA 4Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 5Space Sciences Institute, 4750 Walnut Street, Suite 205, Boulder, CO, USA 6National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ, 85719, USA 7Portland State University, 1825 SW Broadway Portland, OR 97207, USA 8Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA 9Department of Physics, State University of New York at Fredonia, 280 Central Ave, Fredonia, NY 14063, USA 10Space Telescope Science Institute, Baltimore, MD 21218, USA 11Max-Planck-Institute for Astronomy, K¨onigstuhl17, D-69117 Heidelberg, Germany 12Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA 13National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA (Received ...; Revised ...; Accepted May 13, 2020) Submitted to ApJ ABSTRACT We explore the relation between the stellar mass surface density and the mass surface density of molecular hydrogen gas in twelve nearby molecular clouds that are located at <1.5 kpc distance.
  • Binocular Challenge Here

    Binocular Challenge Here

    AHSP Binocular Observing Award Compiled by Phil Harrington www.philharrington.net • To qualify for the BOA pin, you must see 15 of the following 20 binocular targets. Check off each as you spot them. Seen # Object Const. Type* RA Dec Mag Size Nickname 1. M13 Her GC 16 41.7 +36 28 5.9 16' Great Hercules Globular 2. M57 Lyr PN 18 53.6 +33 02 9.7 86"x62" Ring Nebula 3. Collinder 399 Vul AS 19 25.4 +20 11 3.6 60' Coathanger/Brocchi’s Cluster 3.1 4. Albireo Cyg Dbl 19 30.7 +27 57 35” Color Contrasting Double 5.1 5. M27 Vul PN 19 59.6 +22 43 8.1 8’x6’ Dumbbell Nebula 6. NGC 6992 Cyg SNR 20 56.4 +31 43 - 60'x8 Veil Nebula (east) 7. NGC 7000 Cyg BN 20 58.8 +44 20 - 120'x100' North America Nebula 8. M15 Peg GC 21 30.0 +12 10 7.5 12’ Great Pegasus Cluster 9. M39 Cyg OC 21 32.2 +48 26 4.6 32' 10. Barnard 168 Cyg DN 21 53.2 +47 12 - 100'x10' West of Cocoon Nebula 11. IC 5146 Cyg BN/OC 21 53.5 +47 16 - 12'x12' Cocoon Nebula 12. M110 And Gx 00 40.4 +41 41 10 17’x10’ 13. M32 And Gx 00 42.8 +40 52 10 8’x6’ 14. M31 And Gx 00 42.8 +41 16 4.5 178’ Andromeda Galaxy 15. NGC 457 Cas OC 01 19.1 +58 20 6.4 13’ Owl Cluster/ET Cluster 16.
  • September 2020 BRAS Newsletter

    September 2020 BRAS Newsletter

    A Neowise Comet 2020, photo by Ralf Rohner of Skypointer Photography Monthly Meeting September 14th at 7:00 PM, via Jitsi (Monthly meetings are on 2nd Mondays at Highland Road Park Observatory, temporarily during quarantine at meet.jit.si/BRASMeets). GUEST SPEAKER: NASA Michoud Assembly Facility Director, Robert Champion What's In This Issue? President’s Message Secretary's Summary Business Meeting Minutes Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night Member’s Corner –My Quest For A Dark Place, by Chris Carlton Astro-Photos by BRAS Members Messages from the HRPO REMOTE DISCUSSION Solar Viewing Plus Night Mercurian Elongation Spooky Sensation Great Martian Opposition Observing Notes: Aquila – The Eagle Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 27 September 2020 President’s Message Welcome to September. You may have noticed that this newsletter is showing up a little bit later than usual, and it’s for good reason: release of the newsletter will now happen after the monthly business meeting so that we can have a chance to keep everybody up to date on the latest information. Sometimes, this will mean the newsletter shows up a couple of days late. But, the upshot is that you’ll now be able to see what we discussed at the recent business meeting and have time to digest it before our general meeting in case you want to give some feedback. Now that we’re on the new format, business meetings (and the oft neglected Light Pollution Committee Meeting), are going to start being open to all members of the club again by simply joining up in the respective chat rooms the Wednesday before the first Monday of the month—which I encourage people to do, especially if you have some ideas you want to see the club put into action.
  • Far-Infrared Observations of a Massive Cluster Forming in the Monoceros R2 filament Hub? T

    Far-Infrared Observations of a Massive Cluster Forming in the Monoceros R2 filament Hub? T

    Astronomy & Astrophysics manuscript no. monr2_hobys˙final˙corrected c ESO 2017 December 5, 2017 Far-infrared observations of a massive cluster forming in the Monoceros R2 filament hub? T. S. M. Rayner1??, M. J. Griffin1, N. Schneider2; 3, F. Motte4; 5, V. K¨onyves5, P. Andr´e5, J. Di Francesco6, P. Didelon5, K. Pattle7, D. Ward-Thompson7, L. D. Anderson8, M. Benedettini9, J.-P. Bernard10, S. Bontemps3, D. Elia9, A. Fuente11, M. Hennemann5, T. Hill5; 12, J. Kirk7, K. Marsh1, A. Men'shchikov5, Q. Nguyen Luong13; 14, N. Peretto1, S. Pezzuto9, A. Rivera-Ingraham15, A. Roy5, K. Rygl16, A.´ S´anchez-Monge2, L. Spinoglio9, J. Tig´e17, S. P. Trevi~no-Morales18, and G. J. White19; 20 1 Cardiff School of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff, Wales, CF24 3AA, UK 2 I. Physik. Institut, University of Cologne, 50937 Cologne, Germany 3 Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, all´eeG. Saint-Hilaire, 33615 Pessac, France 4 Universit´eGrenoble Alpes, CNRS, Institut de Planetologie et d'Astrophysique de Grenoble, 38000 Grenoble, France 5 Laboratoire AIM, CEA/IRFU { CNRS/INSU { Universit´eParis Diderot, CEA-Saclay, 91191 Gif-sur-Yvette Cedex, France 6 NRC, Herzberg Institute of Astrophysics, Victoria, Canada 7 Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK 8 Department of Physics and Astronomy, West Virginia University, Morgantown, WV 26506, USA 9 INAF { Istituto di Astrofisica e Planetologia Spaziali, via Fosso del Cavaliere 100, I-00133 Roma, Italy 10
  • Data Delivery Document

    Data Delivery Document

    The CygnusX Legacy Project Data Description: Delivery 1: July 2011 CygnusX team: Joseph L. Hora1 (PI), Sylvain Bontemps2, Tom Megeath3, Nicola Schneider4 , Frederique Motte4, Sean Carey5, Robert Simon6, Eric Keto1, Howard Smith1, Lori Allen7, Rob Gutermuth8, Giovanni Fazio1, Kathleen Kraemer9, Don Mizuno10, Stephan Price9, Joseph Adams11, Xavier Koenig12 1Harvard-Smithsonian Center for Astrophysics, 2Observatoire de Bordeaux, 3University of Toledo, 4CEA-Saclay, 5Spitzer Science Center, 6Universität zu Köln, 7NOAO, 8Smith College, 9Air Force Research Lab, 10Boston College, 11Cornell University, 12Goddard Space Flight Center Table of Contents 1. Project Summary ..................................................................................................................... 3 1.1 IRAC observations ........................................................................................................... 3 1.2 MIPS observations ........................................................................................................... 4 1.3 Data reduction .................................................................................................................. 5 1.3.1 IRAC reduction ......................................................................................................... 5 1.3.2 MIPS reduction ......................................................................................................... 7 2. Point Source Catalog..............................................................................................................
  • Discovery of a Wolf–Rayet Star Through Detection of Its Photometric Variability

    Discovery of a Wolf–Rayet Star Through Detection of Its Photometric Variability

    The Astronomical Journal, 143:136 (6pp), 2012 June doi:10.1088/0004-6256/143/6/136 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. DISCOVERY OF A WOLF–RAYET STAR THROUGH DETECTION OF ITS PHOTOMETRIC VARIABILITY Colin Littlefield1, Peter Garnavich2, G. H. “Howie” Marion3,Jozsef´ Vinko´ 4,5, Colin McClelland2, Terrence Rettig2, and J. Craig Wheeler5 1 Law School, University of Notre Dame, Notre Dame, IN 46556, USA 2 Physics Department, University of Notre Dame, Notre Dame, IN 46556, USA 3 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA 4 Department of Optics, University of Szeged, Hungary 5 Astronomy Department, University of Texas, Austin, TX 78712, USA Received 2011 November 9; accepted 2012 April 4; published 2012 May 2 ABSTRACT We report the serendipitous discovery of a heavily reddened Wolf–Rayet star that we name WR 142b. While photometrically monitoring a cataclysmic variable, we detected weak variability in a nearby field star. Low- resolution spectroscopy revealed a strong emission line at 7100 Å, suggesting an unusual object and prompting further study. A spectrum taken with the Hobby–Eberly Telescope confirms strong He ii emission and an N iv 7112 Å line consistent with a nitrogen-rich Wolf–Rayet star of spectral class WN6. Analysis of the He ii line strengths reveals no detectable hydrogen in WR 142b. A blue-sensitive spectrum obtained with the Large Binocular Telescope shows no evidence for a hot companion star. The continuum shape and emission line ratios imply a reddening of E(B − V ) = 2.2–2.6 mag.
  • Übersicht NGC-Objektauswahl Cepheus Zur Übersichtskarte

    Übersicht NGC-Objektauswahl Cepheus Zur Übersichtskarte

    NGC-Objektauswahl Cepheus NGC 40 NGC 7055 NGC 7354 NGC 188 NGC 7076 NGC 7380 NGC 1184 NGC 7129 NGC 7419 NGC 1544 NGC 7139 NGC 7423 NGC 2276 NGC 7142 NGC 7429 NGC 2300 NGC 7160 NGC 7510 NGC 6939 NGC 7226 NGC 7538 NGC 6949 NGC 7235 NGC 7708 NGC 6951 NGC 7261 NGC 7762 NGC 7023 NGC 7281 NGC 7822 Sternbild- Übersicht Zur Objektauswahl: Nummer anklicken Zur Übersichtskarte: Objekt anklicken Sternbildübersicht Auswahl NGC 40_7708 Aufsuchkarte Auswahl NGC 188_Aufsuchkarte 2 UMi 2 Auswahl NGC 1184 Aufsuchkarte Auswahl NGC 1544_2276_2300 Aufsuchkarte Auswahl NGC 6939 Aufsuchkarte Auswahl NGC 6949_6951 Aufsuchkarte Auswahl NGC 7023 Aufsuchkarte Auswahl NGC 7055 Aufsuchkarte Auswahl NGC 7076 Aufsuchkarte Auswahl NGC 7129_7142 Aufsuchkarte Auswahl NGC 7139_7160 Aufsuchkarte Auswahl NGC 7226_7235 Aufsuchkarte Auswahl N 7261_7281 Aufsuchkarte Auswahl NGC 7354_7419_7429_7510_7538 Aufsuchkarte Auswahl NGC 7380_7423 Aufsuchkarte Auswahl NGC 7762_7822 Aufsuchkarte Auswahl NGC 40 Übersichtskarte Aufsuch- Auswahl karte NGC 188 Übersichtskarte Aufsuch- Auswahl karte NGC 1184 Übersichtskarte Aufsuch- Auswahl karte NGC 1544 Übersichtskarte Aufsuch- Auswahl karte N 2276_N 2300 Übersichtskarte Aufsuch- Auswahl karte NGC 6939 Übersichtskarte Aufsuch- Auswahl karte NGC 6949 Übersichtskarte Aufsuch- Auswahl karte NGC 6951 Übersichtskarte Aufsuch- Auswahl karte NGC 7023 Übersichtskarte Aufsuch- Auswahl karte NGC 7055 Übersichtskarte Aufsuch- Auswahl karte NGC 7076 Übersichtskarte Aufsuch- Auswahl karte NGC 7129_7142 Übersichtskarte Aufsuch- Auswahl karte NGC 7139