Rings and Echoes: an Overview (Of SN 1987A's Environment)
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A Morpho-Kinematic and Spectroscopic Study of the Bipolar Nebulae: M 2−9, Mz 3, and Hen 2−104
A&A 582, A60 (2015) Astronomy DOI: 10.1051/0004-6361/201526585 & © ESO 2015 Astrophysics A morpho-kinematic and spectroscopic study of the bipolar nebulae: M 2−9, Mz 3, and Hen 2−104 N. Clyne1;2, S. Akras2, W. Steffen3, M. P. Redman1, D. R. Gonçalves2, and E. Harvey1 1 Centre for Astronomy, School of Physics, National University of Ireland Galway, University Road, Galway, Ireland e-mail: [n.clyne1; matt.redman]@nuigalway.ie 2 Observatório do Valongo, Universidade Federal do Rio de Janeiro, Ladeira Pedro Antonio 43, 20080-090 Rio de Janeiro, Brazil 3 Instituto de Astronomía, Universidad Nacional Autónoma de México, Ensenada, B.C., Mexico Received 22 May 2015 / Accepted 26 July 2015 ABSTRACT Context. Complex bipolar shapes can be generated either as a planetary nebula or a symbiotic system. The origin of the material ionised by the white dwarf is very different in these two scenarios, and it complicates the understanding of the morphologies of planetary nebulae. Aims. The physical properties, structure, and dynamics of the bipolar nebulae, M 2−9, Mz 3, and Hen 2−104, are investigated in detail with the aim of understanding their nature, shaping mechanisms, and evolutionary history. Both a morpho-kinematic study and a spectroscopic analysis, can be used to more accurately determine the kinematics and nature of each nebula. Methods. Long-slit optical echelle spectra are used to investigate the morpho-kinematics of M 2−9, Mz 3, and Hen 2−104. The morpho-kinematic modelling software SHAPE is used to constrain both the morphology and kinematics of each nebula by means of detailed 3D models. -
Abstracts of Talks 1
Abstracts of Talks 1 INVITED AND CONTRIBUTED TALKS (in order of presentation) Milky Way and Magellanic Cloud Surveys for Planetary Nebulae Quentin A. Parker, Macquarie University I will review current major progress in PN surveys in our own Galaxy and the Magellanic clouds whilst giving relevant historical context and background. The recent on-line availability of large-scale wide-field surveys of the Galaxy in several optical and near/mid-infrared passbands has provided unprecedented opportunities to refine selection techniques and eliminate contaminants. This has been coupled with surveys offering improved sensitivity and resolution, permitting more extreme ends of the PN luminosity function to be explored while probing hitherto underrepresented evolutionary states. Known PN in our Galaxy and LMC have been significantly increased over the last few years due primarily to the advent of narrow-band imaging in important nebula lines such as H-alpha, [OIII] and [SIII]. These PNe are generally of lower surface brightness, larger angular extent, in more obscured regions and in later stages of evolution than those in most previous surveys. A more representative PN population for in-depth study is now available, particularly in the LMC where the known distance adds considerable utility for derived PN parameters. Future prospects for Galactic and LMC PN research are briefly highlighted. Local Group Surveys for Planetary Nebulae Laura Magrini, INAF, Osservatorio Astrofisico di Arcetri The Local Group (LG) represents the best environment to study in detail the PN population in a large number of morphological types of galaxies. The closeness of the LG galaxies allows us to investigate the faintest side of the PN luminosity function and to detect PNe also in the less luminous galaxies, the dwarf galaxies, where a small number of them is expected. -
III. the S106 Molecular Cloud As Part of the Cygnus X Cloud Complex
A&A 474, 873–882 (2007) Astronomy DOI: 10.1051/0004-6361:20077540 & c ESO 2007 Astrophysics A multiwavelength study of the S106 region III. The S106 molecular cloud as part of the Cygnus X cloud complex N. Schneider1,4,R.Simon4, S. Bontemps2, F. Comerón3, and F. Motte1 1 DAPNIA/SAp CEA/DSM, Laboratoire AIM CNRS - Université Paris Diderot, 91191 Gif-sur-Yvette, France e-mail: [email protected] 2 OASU/LAB-UMR5804, CNRS, Université Bordeaux 1, 33270 Floirac, France 3 ESO, Karl-Schwarzschild Str. 2, 85748 Garching, Germany 4 I. Physikalisches Institut, Universität zu Köln, Zülpicher Straße 77, 50937 Köln, Germany Received 26 March 2007 / Accepted 15 August 2007 ABSTRACT Context. The distance to the wellknown bipolar nebula S106 and its associated molecular cloud is highly uncertain. Values between 0.5 and 2 kpc are given in the literature, favoring a view of S106 as an isolated object at a distance of 600 pc as part of the “Great Cygnus Rift”. However, there is evidence that S106 is physically associated with the Cygnus X complex at a distance of ∼1.7 kpc (Schneider et al. 2006, A&A, 458, 855). In this case, S106 is a more massive and more luminous star forming site than previously thought. Aims. We aim to understand the large-scale distribution of molecular gas in the S106 region, its possible association with other clouds in the Cygnus X south region, and the impact of UV radiation on the gas. This will constrain the distance to S106. Methods. We employ a part of an extended 13CO and C18O1→ 0 survey, performed with the FCRAO, and data from the MSX and Spitzer satellites to study the spatial distribution and correlation of molecular cloud/PDR interfaces in Cygnus X south. -
A Survey of Irradiated Pillars, Globules, and Jets in the Carina Nebula P
A Survey of Irradiated Pillars, Globules, and Jets in the Carina Nebula P. Hartigan 1, M. Reiter 2 N. Smith 2, J. Bally 3, ABSTRACT We present wide-field, deep narrowband H2, Brγ,Hα, [S II], [O III], and broadband I and K-band images of the Carina star formation region. The new images provide a large-scale overview of all the H2 and Brγ emission present in over a square degree centered on this signature star forming complex. By comparing these images with archival HST and Spitzer images we observe how intense UV radiation from O and B stars affects star formation in molecular clouds. We use the images to locate new candidate outflows and identify the principal shock waves and irradiated interfaces within dozens of distinct areas of star-forming activity. Shocked molecular gas in jets traces the parts of the flow that are most shielded from the intense UV radiation. Combining the H2 and optical images gives a more complete view of the jets, which are sometimes only visible in H2. The Carina region hosts several compact young clusters, and the gas within these clusters is affected by radiation from both the cluster stars and the massive stars nearby. The Carina Nebula is ideal for studying the physics of young H II regions and PDR's, as it contains multiple examples of walls and irradiated pillars at various stages of development. Some of the pillars have detached from their host molecular clouds to form proplyds. Fluorescent H2 outlines the interfaces between the ionized and molecular gas, and after removing continuum, we detect spatial offsets between the Brγ and H2 emission along the irradiated interfaces. -
Planetary Nebulae: Observational Properties, Mimics and Diagnostics
CSIRO PUBLISHING www.publish.csiro.au/journals/pasa Publications of the Astronomical Society of Australia, 2010, 27, 129–148 Planetary Nebulae: Observational Properties, Mimics and Diagnostics David J. FrewA,C,D and Quentin A. ParkerA,B A Department of Physics, Macquarie University, North Ryde, NSW 2109 B Anglo–Australian Observatory, Epping, NSW 1710 C Perth Observatory, Bickley, WA 6076 D Corresponding author. Email: [email protected] Received 2009 July 19, accepted 2010 January 21 Abstract: The total number of true, likely and possible planetary nebulae (PN) now known in the Milky Way is nearly 3000, double the number known a decade ago. The new discoveries are a legacy of the recent availability of wide field, narrowband imaging surveys, primarily in the light of H-alpha. In this paper, we summarise the various PN discovery techniques, and give an overview of the many types of objects which mimic PN and which appear as contaminants in both Galactic and extragalactic samples. Much improved discrimination of classical PN from their mimics is now possible based on the wide variety of high-quality multiwavelength data sets that are now available. We offer improved taxonomic and observational definitions for the PN phenomenon based on evaluation of these better diagnostic capabilities. However, we note that evidence is increasing that the PN phenomenon is heterogeneous, and PN are likely to be formed from multiple evolutionary scenarios. In particular, the relationships between some collimated symbiotic outflows and bipolar PN remain uncertain. Keywords: catalogs — planetary nebulae: general — stars: AGB and post-AGB — stars: fundamental parameters — surveys — techniques: photometric, spectroscopic 1 Introduction The total number of currently known Galactic PN is A classical planetary nebula (PN) is a shell of ionized nearly 3000, which includes all known confirmed PN from gas, ejected from a star of low to intermediate mass (∼1 the catalogues of Acker et al. -
THE STAR FORMATION NEWSLETTER an Electronic Publication Dedicated to Early Stellar Evolution and Molecular Clouds
THE STAR FORMATION NEWSLETTER An electronic publication dedicated to early stellar evolution and molecular clouds No. 192 — 6 Dec 2008 Editor: Bo Reipurth ([email protected]) Special Issue Handbook of Star Forming Regions Edited by Bo Reipurth The Handbook describes the ∼60 most important star forming regions within approximately 2 kpc, and has been written by a team of 105 authors with expertise in the individual regions. It consists of two full color volumes, one for the northern and one for the southern hemisphere, with a total of over 1900 pages. The Handbook aims to be a source of comprehensive factual information about each region, with very extensive references to the literature. The development of our understanding of a given region is outlined, and hence many of the earliest studies are, if not discussed, then at least mentioned, even if they are only of historical interest today. Young low- and high-mass populations are discussed, as well as the molecular and ionized gas. The text is supported by extensive use of figures and tables. Authors have been encouraged to complete their chapters with a section on individual objects of special interest. Little emphasis is placed on more general discussions of star formation processes and the properties of young stars, subjects that are well covered elsewhere. The Handbook will thus serve as a reference guide for researchers and students embarking on a study of one or more of these regions, and will hopefully also inspire new work to be done where information is clearly missing. In order to keep the Handbook within some reasonable limits, it was from the beginning decided to limit regions to those closer than approximately 2 kpc. -
The Influence of Massive Stars in the Interstellar Medium of IC 1613: The
The influence of massive stars in the interstellar medium of IC 1613: the supernova remnant S8 and the nebula S3 associated with a WO star. M. Rosado1, M. Valdez-Guti´errez2, L. Georgiev1, L. Arias1, J. Borissova3 and R. Kurtev3 ABSTRACT We present a detailed kinematical analysis of two selected nebulae in the Local Group irregular galaxy IC 1613. The nebulae are: S8 (Sandage 1971), the only known supernova remnant in this galaxy, and S3, a Wolf-Rayet nebula associated with the only WO star in this galaxy. For S8, we have obtained and analyzed its radial velocity field, where we found complex profiles which can be fitted by several velocity components. These profiles also show the presence of high velocity, low density gas. From this, we have obtained the expansion velocity, estimated the preshock density and calculated the basic kinematical parameters of this SNR. We suggest that in S8 we are seing a SNR partially hidden by dust. This suggestion comes from the fact that the SNR is located between two superbubbles where a ridge of obscured material unveils the existence of dust. Moreover, we show that this hypothesis prevails when energetic arguments are taken into account. In the case of S3, this nebula shows bipolar structure. By means of its kinematics, we have analyzed its two lobes, the “waist”, as well as its relation with the nearest superbubbles. For the first time we are able to see closed the NW lobe, showing a clover leaf shape. This fact allows a better quantitative knowledge of the nebula as a whole. -
Binary Planetary Nebulae Nuclei Towards the Galactic Bulge II
A&A 505, 249–263 (2009) Astronomy DOI: 10.1051/0004-6361/200912176 & c ESO 2009 Astrophysics Binary planetary nebulae nuclei towards the Galactic bulge II. A penchant for bipolarity and low-ionisation structures B. Miszalski1,2, A. Acker1,Q.A.Parker2,3,andA.F.J.Moffat4 1 Observatoire Astronomique, Université de Strasbourg, 67000, Strasbourg, France e-mail: [brent;acker]@newb6.u-strasbg.fr 2 Department of Physics, Macquarie University, Sydney, NSW 2109, Australia e-mail: [brent;qap]@ics.mq.edu.au 3 Anglo-Australian Observatory, Epping, NSW 1710, Australia 4 Dépt. de physique, Univ. de Montréal CP 6128, Succ. Centre-Ville, Montréal, QC H3C 3J7, and Centre de recherche en astrophysique du Québec, Canada e-mail: [email protected] Received 25 March 2009 / Accepted 7 July 2009 ABSTRACT Considerable effort has been applied towards understanding the precise shaping mechanisms responsible for the diverse range of morphologies exhibited by planetary nebulae (PNe). At least 10–20% of PNe have central stars (CSPN) with a close binary companion thought responsible for heavily shaping the ejected PN during common-envelope (CE) evolution, however morphological studies of the few available examples found no clear distinction between PNe and post-CE PNe. The discovery of several new binary central stars (CSPN) from the OGLE-III photometric variability survey has significantly increased the number of post-CE PNe available for morphological analysis to 30 PNe. High quality Gemini South narrow-band images are presented for most of the OGLE sample, while some previously known post-CE PNe are reanalysed with images from the literature. -
Thepapillon'nebula: a Compact HII Blob in the LMC Resolved By
A&A manuscript no. ASTRONOMY (will be inserted by hand later) AND Your thesaurus codes are: 3(08.05.1; 09.04.1; 09.08.1; 09.09.1 N159-5; 09.11.1; 11.13.1) ASTROPHYSICS The “Papillon” nebula: a compact H ii blob in the LMC resolved by HST ⋆ M. Heydari-Malayeri1, M.R. Rosa2, ⋆⋆, V. Charmandaris1, L. Deharveng3, and H. Zinnecker4 1 demirm, Observatoire de Paris, 61 Avenue de l’Observatoire, F-75014 Paris, France 2 Space Telescope European Coordinating Facility, European Southern Observatory, Karl-Schwarzschild-Strasse-2, D-85748 Garching bei M¨unchen, Germany 3 Observatoire de Marseille, 2 Place Le Verrier, F-13248 Marseille Cedex 4, France 4 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany Received 11 June 1999 / Accepted 12 July 1999 Abstract. We present high spatial resolution HST imag- the mass of the star (Yorke & Kr¨ugel 1977, Wolfire & ing of the LMC compact H ii region N159-5. This high Cassinelli 1987, Beech & Mitalas 1994), while a large frac- excitation blob is revealed to be a “papillon” or butterfly- tion of the infalling material may as well be deflected into shaped ionized nebula with the “wings” separated by bipolar outflows by processes which we do not yet know ∼ 2′′.3 (0.6 pc). Two subarcsecond features resembling a in detail (Churchwell 1997). “smoke ring” and a “globule” are detected in the wings, Moreover, since the evolutionary time scales of mas- the origin of which is briefly discussed. N159-5 may rep- sive stars are comparatively short, these stars are be- resent a new type of H ii region in the Magellanic Clouds lieved to enter the main sequence while still embedded overlooked so far because of insufficient spatial resolu- in their parent molecular clouds (Yorke & Kr¨ugel 1977, tion. -
Herschel⋆ Far-Infrared Observations of the Carina Nebula Complex⋆⋆
A&A 554, A6 (2013) Astronomy DOI: 10.1051/0004-6361/201321081 & c ESO 2013 Astrophysics Herschel far-infrared observations of the Carina Nebula complex III. Detailed cloud structure and feedback effects V. Roccatagliata, T. Preibisch, T. Ratzka, and B. Gaczkowski Universitäts-Sternwarte München, Ludwig-Maximilians-Universität, Scheinerstr. 1, 81679 München, Germany e-mail: [email protected] Received 11 January 2013 / Accepted 19 March 2013 ABSTRACT Context. The star formation process in large clusters/associations can be strongly influenced by the feedback from high-mass stars. Whether the resulting net effect of the feedback is predominantly negative (cloud dispersal) or positive (triggering of star formation due to cloud compression) is still an open question. Aims. The Carina Nebula complex (CNC) represents one of the most massive star-forming regions in our Galaxy. We use our Herschel far-infrared observations to study the properties of the clouds over the entire area of the CNC (with a diameter of ≈3.2◦,which corresponds to ≈125 pc at a distance of 2.3 kpc). The good angular resolution (10−36)oftheHerschel maps corresponds to physical scales of 0.1–0.4 pc, and allows us to analyze the small-scale (i.e., clump-size) structures of the clouds. Methods. The full extent of the CNC was mapped with PACS and SPIRE in the 70, 160, 250, 350, and 500 μm bands. We determined temperatures and column densities at each point in these maps by modeling the observed far-infrared spectral energy distributions. We also derived a map showing the strength of the UV radiation field. -
A Herschel Study of NGC 650⋆⋆⋆
A&A 560, A7 (2013) Astronomy DOI: 10.1051/0004-6361/201221023 & c ESO 2013 Astrophysics A Herschel study of NGC 650?;?? P. A. M. van Hoof1, G. C. Van de Steene1, K. M. Exter2, M. J. Barlow3, T. Ueta4, M. A. T. Groenewegen1, W. K. Gear5, H. L. Gomez5, P. C. Hargrave5, R. J. Ivison6, S. J. Leeks7, T. L. Lim7, G. Olofsson8, E. T. Polehampton7;9, B. M. Swinyard7, H. Van Winckel2, C. Waelkens2, and R. Wesson3 1 Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium e-mail: [email protected] 2 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium 3 Dept of Physics & Astronomy, University College London, Gower St, London WC1E 6BT, UK 4 Dept. of Physics and Astronomy, University of Denver, Mail Stop 6900, Denver, CO 80208, USA 5 School of Physics and Astronomy, Cardiff University, 5 The Parade, Cardiff, Wales CF24 3YB, UK 6 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK 7 Space Science and Technology Department, Rutherford Appleton Laboratory, Oxfordshire, OX11 0QX, UK 8 Dept. of Astronomy, Stockholm University, AlbaNova University Center, Roslagstullsbacken 21, 10691 Stockholm, Sweden 9 Department of Physics, University of Lethbridge, Lethbridge, Alberta, T1J 1B1, Canada Received 31 December 2012 / Accepted 26 July 2013 ABSTRACT As part of the Herschel guaranteed time key project Mass loss of Evolved StarS (MESS) we have imaged a sample of planetary nebulae. In this paper we present the Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) images of the classical bipolar planetary nebula NGC 650. -
Cycle 10 Abstract Catalog (Based on Phase I Submissions)
Cycle 10 Abstract catalog (based on Phase I submissions) ================================================================================ Proposal Category: GO Scientific Category: Cosmology ID: 9033 Title: Measuring the mass distribution in the most distant, very X-ray luminous galaxy cluster known PI: Harald Ebeling PI Institution: Institute for Astronomy We propose to obtain a mosaic of deep HST/WFPC2 images to conduct a weak lensing analysis of the mass distribution in the massive, distant galaxy cluster ClJ1226.9+3332, recently discovered by us. At z=0.888 this exceptional system is more X-ray luminous and more distant than both MS1054.4-0321 and ClJ0152.7-1357, the previous record holders, thus providing yet greater leverage for cosmological studies of cluster evolution. ClJ1226.9+3332 differs markedly from all other currently known distant clusters in that it exhibits little substructure and may even host a cooling flow, suggesting that it could be the first cluster to be discovered at high redshift that is virialized. We propose joint HST and Chandra observations to investigate the dynamical state of this extreme object. This project will 1) take advantage of HST's superb resolution at optical wavelengths to accurately map the mass distribution within 1.9 h^-1_ 50 Mpc via strong and weak gravitational lensing, and 2) use Chandra's unprecedented resolution in the X-ray waveband to obtain independent constraints on the gas and dark matter distribution in the cluster core, including the suspected cooling flow region. As a bonus, the proposed WFPC2 observations will allow us to test the results by van Dokkum et al. (1998, 1999) on the properties of cluster galaxies (specifically merger rate and morphologies) at z~ 0.8 from their HST study of MS1054.4-0321.