Swayamtrupta Panda National Institute of Technology Rourkela, India

Slides:



Advertisements
Similar presentations
Physical conditions of the shocked regions in collimated outflows of planetary nebulae Angels Riera (UPC)
Advertisements

Spectro-imaging observations of H 3 + on Jupiter Observatoire de Paris, France Emmanuel Lellouch.
Lyα Pumped Molecular Hydrogen Emission in the Planetary Nebulae NGC 6853 and NGC 3132 R.E. Lupu, K. France and S.R. McCandliss Johns Hopkins University,
The Nature and Origin of Molecular Knots in Planetary Nebulae Sarah Eyermann – U. of Missouri Angela Speck – U. of Missouri Margaret Meixner – STScI Peter.
The morphology and kinematics of planetary nebulae: a tribute to Hugo Schwarz Romano L.M. Corradi Isaac Newton Group of Telescopes.
Other Planetary Systems (Chapter 13) Extrasolar Planets
MOLECULAR GAS and DUST at the CENTER of the EGG NEBULA Jeremy Lim and Dinh-V-Trung (Institute of Astronomy & Astrophysics, Academia Sinica, Taiwan) Introduction.
X-ray Emission from PNe Martín A. Guerrero You-Hua Chu Robert A. Gruendl Univ. of Illinois APN III, Mt Rainier, 7/30/03.
Spitzer/IRS survey of heavily obscured planetary nebula precursors planetary nebula precursors D. A. García-Hernández (McDonald Observatory, UT, USA) J.
A101 Slide Set: Young Galaxies Grow Developed by the GALEX Team 1 Topic: Galaxies Concepts: Ultraviolet observations, galaxy formation, galaxy evolution,
A new class of warm debris disks? Rachel Smith, Institute for Astronomy; Mark Wyatt, Abstract.
Multiwavelength Continuum Survey of Protostellar Disks in Ophiuchus Left: Submillimeter Array (SMA) aperture synthesis images of 870 μm (350 GHz) continuum.
Black holes: do they exist?
P olarized R adiation I maging and S pectroscopy M ission Probing cosmic structures and radiation with the ultimate polarimetric spectro-imaging of the.
The Death of a Low Mass Star n Evolution of a sun-like star post helium- flash –The star moves onto the horizontal branch of the Hertzprung-Russell diagram.
ASTR112 The Galaxy Lecture 8 Prof. John Hearnshaw 12. The interstellar medium (ISM): gas 12.1 Types of IS gas cloud 12.2 H II regions (diffuse gaseous.
What can we learn from the luminosity function and color studies? THE SDSS GALAXIES AT REDSHIFT 0.1.
Molecular Gas and Dust in SMGs in COSMOS Left panel is the COSMOS field with overlays of single-dish mm surveys. Right panel is a 0.3 sq degree map at.
1 GALEX Angular Correlation Function … or about the Galactic extinction effects.
The Close Binary Central Star of the Young Planetary Nebula HB12 C. H. Hsia a, W. H. Ip a, J.Y. Hu b a Institute of Astronomy, National Central University,
The Evolution of Quasars and Massive Black Holes “Quasar Hosts and the Black Hole-Spheroid Connection”: Dunlop 2004 “The Evolution of Quasars”: Osmer 2004.
Richard Mushotzky (NASA/GSFC) and Amalia K. Hicks (University of Colorado) An enduring enigma in X-ray astronomy is the "missing mass" in cooling flow.
Pedro GARCIA-LARIOPlanetary Nebulae beyond the Milky Way 19-21/05/2004, Page 1 Extragalactic PNe: methods of discovery using infrared photometry Extragalactic.
Chile Sky Background at ESO/la Silla in the Visible and Near IR Leonardo Vanzi -Olivier R. Hainaut European Southern Observatory La Silla - Chile.
Multi-slit spectroscopy In sky-noise dominated conditions (most interesting!) the use of slits is essential: eg: Faint object, extra-galactic, surveys:
VLASS – Galactic Science Life cycle of star formation in our Galaxy as a proxy for understanding the Local Universe legacy science Infrared GLIMPSE survey.
Hee-Won Lee ARCSEC and Dept. of Astronomy Sejong University 2010 August 26.
I.Introduction  Recent evidence from Fermi and the VLBA has revealed a strong connection between ɣ -ray emission in AGNs and their parsec-scale radio.
Imaging Molecular Gas in a Nearby Starburst Galaxy NGC 3256, a nearby luminous infrared galaxy, as imaged by the SMA. (Left) Integrated CO(2-1) intensity.
Morphological classification of new candidate PNe in an IPHAS sample Kerttu Viironen IAC Collaboration: A. Mampaso (IAC) R. Corradi (ING, IAC), R. Greimel.
Structure Formation in the Universe Concentrate on: the origin of structure in the Universe How do we make progress?How do we make progress? What are the.
Submillimeter Array CH3OH A Cluster of Highly Collimated and Young Bipolar Outflows Emanating from OMC1 South. Luis A. Zapata 1,2, Luis.
The Prevalence and Properties of Outflowing Galactic Winds at z = 1 Katherine A. Kornei (UCLA) Alice Shapley, Crystal Martin, Alison Coil ETH Zurich February.
ALMA Science Examples Min S. Yun (UMass/ANASAC). ALMA Science Requirements  High Fidelity Imaging  Precise Imaging at 0.1” Resolution  Routine Sub-mJy.
Planetary nebulae beyond the Milky Way - May , Magellanic Cloud planetary nebulae as probes of stellar evolution and populations Letizia Stanghellini.
Methanol Masers in the NGC6334F Star Forming Region Simon Ellingsen & Anne-Marie Brick University of Tasmania Centre for Astrophysics of Compact Objects.
Molecular clouds in the center of M81 Viviana Casasola Observatoire de Paris-LERMA & Università di Padova, Dipartimento di Astronomia Scuola Nazionale.
The circumstellar environment of evolved stars as seen by VLTI / MIDI Keiichi Ohnaka Max-Planck-Institut für Radioastronomie, Infrared Interferometry Group.
Competitive Science with the WHT for Nearby Unresolved Galaxies Reynier Peletier Kapteyn Astronomical Institute Groningen.
Active Galaxies Galaxies with extremely violent energy release in their nuclei (pl. of nucleus). → “Active Galactic Nuclei” (= AGN) Up to many thousand.
Simulations for the nearby Seyfert 2 galaxy NGC 4945 Lien-Hsuan Lin 1,2, Chi Yuan 2, C.C. D. Yen 3, and S. Muller 2 1 Department of Physics, National Taiwan.
Discovery and Characterization of Galactic Ionized Nebulae with WHAM Peter Doze, Texas Southern University Advisor: Dr. Bob Benjamin University of Wisconsin-Madison.
Wide-field Infrared Survey Explorer (WISE) is a NASA infrared- wavelength astronomical space telescope launched on December 14, 2009 It’s an Earth-orbiting.
Color Magnitude Diagram VG. So we want a color magnitude diagram for AGN so that by looking at the color of an AGN we can get its luminosity –But AGN.
Stellar evolution in the post-AGB stage Olga Suárez Laboratorio de Astrofísica Espacial y Física Fundamental – Madrid (Spain) Supervisors: Minia Manteiga.
Observations of Bipolar planetary nebulae at 30 Micron Kentaro Asano (Univ.Tokyo) Takashi Miyata, Shigeyuki Sako, Takafumi Kamizuka, Tomohiko Nakamura,
Globular Clusters Globular clusters are clusters of stars which contain stars of various stages in their evolution. An H-R diagram for a globular cluster.
Netherlands Organisation for Scientific Research High resolution X-ray spectroscopy of the Interstellar Medium (ISM) C. Pinto (SRON), J. S. Kaastra (SRON),
Before it was seen, it was heard. Brainstorming. Star Clusters Chang, Seo-Won.
Spectral classification of galaxies of LAMOST DR3
Tracing the coronal emission in AGN with VLT/NACO
SN 1987A: The Formation & Evolution of Dust in a Supernova Explosion
H Stacked Images Reveal Large Numbers of PNe in the LMC
An Arecibo HI 21-cm Absorption Survey of Rich Abell Clusters
A Galaxy Revealed in Multiple Wavelengths
WASP-12.
GALEX: Galaxy Evolution Explorer
Our Milky Way Galaxy.
Stars.
Infrared study of a star forming region, L1251B
The Stellar Population of Metal−Poor Galaxies at z~1
The dust attenuation in the galaxy merger Mrk848
HST Surveys of the LMC Planetary Nebulae
The Interstellar Medium
Planetary Nebula abundances in NGC 5128 with FORS
Millimeter Megamasers and AGN Feedback
EVN observations of OH maser burst in OH
The region N of the SMC The region N of the SMC. Possible supernova explosions and triggered star formation Emmanuel.
Borislav Nedelchev et al. 2019
Presentation transcript:

GALEX Observations of Planetary Nebulae: Estimating their Angular Sizes Swayamtrupta Panda National Institute of Technology Rourkela, India Collaborators: Ananta C. Pradhan1 (Project Supervisor), M. Parthasararathy2, Jayant Murthy3, D.K. Ojha4 1 National Institute of Technology, Rourkela, India; 2 Inter-University Centre for Astronomy and Astrophysics, Pune, India; 3 Indian Institute of Astrophysics, Bangalore, India; 4 Tata Institute for Fundamental Research, Mumbai, India Abstract: PNe distribution by GALEX: IUE Spectra of a PN: The ultraviolet spectral regions (1200-3200 Å) of Planetary Nebulae (PNe) contain important nebular emission lines pertaining to low metallicity hot central stars of planetary nebulae (CSPNe). CSPNe, being hot post-AGB stars, are more easily detected in the UV regime than in the optical. To understand the wavelength dependent PNe morphology, comparing the UV tracing the hot gas in the inner regions of the nebulae to the optical images holds significant importance. The GR6-GR7 data releases of NUV and FUV images from GALEX at 5 arcseconds resolution are used to study large images of PNe where deep sensitivity combined with the low sky background in FUV may reveal faint structures, shock fronts, collimated outflows and morphology. Among these, the angular sizes of PNe, a vital observational entity, is used to determine nebular distances and masses of the PNe. Utilising direct measurements at the 10% level of peak surface brightness, Gaussian deconvolution and second moment deconvolution, we measure the angular dimensions of the PNe. We found several of the PNe that GALEX detected have IUE (International Ultraviolet Explorer) spectra. We have obtained the low dispersion spectrum from SWP01741 and LWR01635 for PN G358.3-21.6, which is a high excitation PN. Since GALEX and IUE have almost similar wavelength coverage, we have shown the filter response curves of GALEX’s FUV and NUV filters on the combined IUE (SWP01741 + LWR01635) spectra (figure 2). The prominent emission lines seen in the spectrum are H I, O V, C IV, He II, CIII], He II, [Mg V], and O III. The emission lines contributing to GALEX FUV flux are strong OV, C IV, and He II while the emission lines contributing to the NUV flux are C III] and He II. Measurement of size of PNe: Figure 1: Distribution of PNe detected by GALEX (shown in an Aitoff projection in Galactic coordinates) We have determined the angular sizes of the PNe in NUV and FUV for whichever sources the detection exists. Initially we used the direct measurements at the 10% level of the peak surface brightness but the GALEX images are very deep and the nebular emission extends beyond the 10% contour. So, we measured the actual dimension of the nebula considering a 3σ emission level above the background. PNe: Introduction IUE spectrum of PN G358.3-21.6: Variation of flux across a PN: ◮ PNe are the end product of the stars of masses between 0.8 M⊙ and 8 M⊙. A planetary nebula (PN) consists of a hot, luminous central star and an expanding glowing shell of gas and dust. ◮ More than 3000 PNe have been detected in the Milky Way which are catalogued by Parker et al. (2006) and Acker et al. (1992). ◮ The central star of most of the PNe (CSPNe) is a very hot object which is bright in UV and hence, the UV observations explore the properties of these objects. Results and Discussions: ◮ The IUE spectra shows that the emission lines contributing to GALEX FUV flux are strong O V, C IV, and He II while the emission lines contributing to the NUV flux are C III] and He II. ◮ x-cut and y-cut across the PN is shown (figure 3). The peak corresponds the intensity of the central star. ◮ PN morphology in UV is different from that in optical as the UV traces the hot gases in the inner region of nebulae. ◮ The NUV and FUV morphologies of a few of the 112 PNe are shown. (figure 4, figure 5) ◮ We found most of the PNe are circular, where 20% are elliptical and 7% are bipolar. ◮ The NUV and FUV size of the PNe (table 1) are different, the NUV sizes are larger than the FUV sizes proving that the FUV extensions are less than that of the NUV. ◮ The bipolar morphology is the result of the interaction of a close binary. ◮ We aim to measure the UV integrated fluxes and distances of the PNe from the UV morphologies. Figure 2: IUE spectrum of PN G358.3-21.6. The blue solid and dashed lines are the effective area curves of GALEX FUV and NUV filters, respectively. Figure 3: X and Y pixel values of a PN is shown here to know its expansion in UV. NUV images of a few PNe: FUV images of a few PNe: Angular sizes of PNe: ◮ The angular size of PN is one of the most important observational entity, which is used in determining nebular distances and masses of the PN. ◮ Several methods such as direct measurements at the 10% level of the peak surface brightness, Gaussian deconvolution, second-moment deconvolution, etc., have been employed to measure the angular dimension of PNe that are observed by various techniques (Tylenda et al. 2003, van Hoof et al. 2000). ◮ We have measured the angular diameter of 112 PNe which were detected by Galaxy Evolution Explorer (GALEX) survey. Figure 4 Figure 5 UV details of a few PNe: GALEX Observations: ◮ GALEX has covered 75% of the sky in two UV bands, FUV and NUV, simultaneously, with spatial resolution of 4.2′′ and 5.3′′, peaking at 1539 Å and 2316 Å, respectively (Morrissey et al. 2007). ◮ We have downloaded all the GALEX GR7 data from MAST archive. ◮ We searched the GALEX data base using the Vizier catalogue of galactic PNe by Acker et al. (1992) and the MASH catalogue of PNe by Parker et al. (2006). We detected a total of 112 PNe in GALEX database using CDS X-Match. ◮ Most of these objects are from the AIS survey except a few, which are from the MIS survey (also from NIS, GII and NGS) of GALEX. However, 39 of the PNe in the list have both FUV and NUV detections. We have shown all the 112 PNe in an Aitoff projection in Galactic coordinates (figure 1). Table 1: Measurements of sizes of a few PNe References [1] Acker A., Marcout J., Ochsenbein F., Stenholm B., Tylenda R., 1992, Strasbourg-ESO catalogue of galactic planetary nebulae (Garching: European Southern Observatory) [2] Morrissey P., Conrow T., Barlow T.A., 2007, ApJS, 173, 682. [3] Parker Q. A., Acker A., Frew D. J., 2006, 373, 79 [4] Tylenda R., Siόdmiak N., Gόrny S. K., Corradi R. L. M., Schwarz H. E., 2003, 405, 627 [5] van Hoof P. A. M., 2000, 314, 99 Last column represents the optical diameters for the PNe