Popular Names of Deep Sky (Galaxies,Nebulae and Clusters) Viciana’S List
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Stsci Newsletter: 1997 Volume 014 Issue 01
January 1997 • Volume 14, Number 1 SPACE TELESCOPE SCIENCE INSTITUTE Highlights of this issue: • AURA science and functional awards to Leitherer and Hanisch — pages 1 and 23 • Cycle 7 to be extended — page 5 • Cycle 7 approved Newsletter program listing — pages 7-13 Astronomy with HST Climbing the Starburst Distance Ladder C. Leitherer Massive stars are an important and powerful star formation events in sometimes dominant energy source for galaxies. Even the most luminous star- a galaxy. Their high luminosity, both in forming regions in our Galaxy are tiny light and mechanical energy, makes on a cosmic scale. They are not them detectable up to cosmological dominated by the properties of an distances. Stars ~100 times more entire population but by individual massive than the Sun are one million stars. Therefore stochastic effects times more luminous. Except for stars prevail. Extinction represents a severe of transient brightness, like novae and problem when a reliable census of the supernovae, hot, massive stars are Galactic high-mass star-formation the most luminous stellar objects in history is atempted, especially since the universe. massive stars belong to the extreme Massive stars are, however, Population I, with correspondingly extremely rare: The number of stars small vertical scale heights. Moreover, formed per unit mass interval is the proximity of Galactic regions — roughly proportional to the -2.35 although advantageous for detailed power of mass. We expect to find very studies of individual stars — makes it few massive stars compared to, say, difficult to obtain integrated properties, solar-type stars. This is consistent with such as total emission-line fluxes of observations in our solar neighbor- the ionized gas. -
Visual Astronomy Filter Research
Visual Astronomy Filter Research by Jim Thompson, P.Eng May 2010 Table of Contents: 1.0 The Great Filter Filibuster ...................................................................................... 3 2.0 The Human Eye...................................................................................................... 5 3.0 Planetary (Colour) Filter Research ......................................................................... 7 4.0 Using Planetary (Colour) Filters........................................................................... 12 5.0 Deep-Sky (Band Pass) Filter Research................................................................. 21 6.0 Using Deep-Sky (Band Pass) Filters..................................................................... 25 7.0 References............................................................................................................. 33 Appendix A – Colour Filter Plots ..................................................................................... 36 Appendix B – Deepsky Filter Plots .................................................................................. 43 List of Figures: Figure 1 An assortment of planetary (colour) filters ...................................................... 3 Figure 2 An example of deep-sky (band-pass) filters..................................................... 4 Figure 3 Human Eye Rod & Cone Density Distribution ................................................ 5 Figure 4 Human Eye Spectral Sensitivity...................................................................... -
Near and Mid-IR Photometry of the Pleiades, and a New List Of
ApJS, in press; version with embedded figures can be obtained at http://spider.ipac.caltech.edu/staff/stauffer/ Near and Mid-IR Photometry of the Pleiades, and a New List of Substellar Candidate Members1,2 John R. Stauffer Spitzer Science Center, Caltech 314-6, Pasadena, CA 91125 [email protected] Lee W. Hartmann Astronomy Department, University of Michigan Giovanni G. Fazio, Lori E. Allen, Brian M. Patten Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 Patrick J. Lowrance, Robert L. Hurt, Luisa M. Rebull Spitzer Science Center, Caltech , Pasadena, CA 91125 Roc M. Cutri, Solange V. Ramirez Infrared Processing and Analysis Center, Caltech 220-6, Pasadena, CA 91125 Erick T. Young, George H. Rieke, Nadya I. Gorlova3, James C. Muzerolle Steward Observatory, University of Arizona, Tucson, AZ 85726 Cathy L. Slesnick Astronomy Department, Caltech, Pasadena, CA 91125 arXiv:0704.1832v1 [astro-ph] 13 Apr 2007 Michael F. Skrutskie Astronomy Department, University of Virginia, Charlottesville, VA 22903 1This work is based (in part) on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. 2This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. 3Current address: University of Florida, 211 Bryant Space Center, Gainesville, FL 32611 –2– ABSTRACT We make use of new near and mid-IR photometry of the Pleiades cluster in order to help identify proposed cluster members. -
PUBLICATIONS Publications (As of Dec 2020): 335 on Refereed Journals, 90 Selected from Non-Refereed Journals. Citations From
PUBLICATIONS Publications (as of Sep 2021): 350 on refereed journals, 92 selected from non-refereed journals. Citations from ADS: 32263, H-index= 97. Refereed 350. Caminha, G.B.; Suyu, S.H.; Grillo, C.; Rosati, P.; et al. 2021 Galaxy cluster strong lensing cosmography: cosmological constraints from a sample of regular galaxy clusters, submitted to A&A 349. Mercurio, A..; Rosati, P., Biviano, A. et al. 2021 CLASH-VLT: Abell S1063. Cluster assembly history and spectroscopic catalogue, submitted to A&A, (arXiv:2109.03305) 348. G. Granata et al. (9 coauthors including P. Rosati) 2021 Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: the case of Abell S1063, submitted to A&A, (arXiv:2107.09079) 347. E. Vanzella et al. (19 coauthors including P. Rosati) 2021 High star cluster formation efficiency in the strongly lensed Sunburst Lyman-continuum galaxy at z = 2:37, submitted to A&A, (arXiv:2106.10280) 346. M.G. Paillalef et al. (9 coauthors including P. Rosati) 2021 Ionized gas kinematics of cluster AGN at z ∼ 0:8 with KMOS, MNRAS, 506, 385 6 crediti 345. M. Scalco et al. (12 coauthors including P. Rosati) 2021 The HST large programme on Centauri - IV. Catalogue of two external fields, MNRAS, 505, 3549 344. P. Rosati et al. 2021 Synergies of THESEUS with the large facilities of the 2030s and guest observer opportunities, Experimental Astronomy, 2021ExA...tmp...79R (arXiv:2104.09535) 343. N.R. Tanvir et al. (33 coauthors including P. Rosati) 2021 Exploration of the high-redshift universe enabled by THESEUS, Experimental Astronomy, 2021ExA...tmp...97T (arXiv:2104.09532) 342. -
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. -
The Evening Sky Map a DECEMBER 2018 N
I N E D R I A C A S T N E O D I T A C L E O R N I G D S T S H A E P H M O O R C I . Z N O n i f d o P t o ) l a h O N r g i u s , o Z l t P h I C e r o N R ( I o r R r O e t p h C H p i L S t D E E a g r i . H ( B T F e O h T NORTH D R t h N e M e E s A G X O U e A H m M C T i . I n P i N d S L E E m P Z “ e E A N Dipper t e H O NORTHERN HEMISPHERE o M T R r T The Big The N Y s H h . E r o ” E K Alcor & e w ) t W S . s e . T u r T Mizar l E U p W C B e R e a N l W D k b E s T u T MAJOR W H o o The Evening Sky Map A DECEMBER 2018 n E C D O t FREE* EACH MONTH FOR YOU TO EXPLORE, LEARN & ENJOY THE NIGHT SKY URSA S e L h K h e t Y E m R d M A n o A a r Thuban S SKY MAP SHOWS HOW P Get Sky Calendar on Twitter n T 1 i n C A 3 E g R M J http://twitter.com/skymaps O Sky Calendar – December 2018 o d B THE NIGHT SKY LOOKS U M13 f n O N i D “ f L D e T DRACO A o c NE O I t I e T EARLY DEC PM T 8 m P t S i 3 Moon near Spica (morning sky) at 9h UT. -
Chemical Composition of the Young Open Clusters IC 2602 and IC 2391 ,
A&A 501, 553–562 (2009) Astronomy DOI: 10.1051/0004-6361/200811587 & c ESO 2009 Astrophysics Chemical composition of the young open clusters IC 2602 and IC 2391, V. D’Orazi1,2 and S. Randich2 1 Dipartimento di Astronomia e Scienza dello Spazio, Università di Firenze, Largo E. Fermi 2, Firenze, Italy e-mail: [email protected] 2 INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, Firenze, Italy Received 23 December 2008 / Accepted 21 April 2009 ABSTRACT Context. Galactic open clusters have been long recognized as one of the best tools to investigate the chemical content of Galactic disk and its time evolution. In the last decade, many efforts have been directed to chemically characterize the old and intermediate age population; surprisingly, the chemical content of the younger and close counterpart remains largely undetermined. Aims. In this paper we present the abundance analysis of a sample of 15 G/K members of the young pre-main sequence clusters IC 2602 and IC 2391. Along with IC 4665, these are the first pre-main sequence clusters for which a detailed abundance determination has been carried out so far. Methods. We analyzed high-resolution, high S/N spectra acquired with different instruments (UVES and CASPEC at ESO, and the echelle spectrograph at CTIO), using MOOG and equivalent width measurements. Along with metallicity ([Fe/H]), we measured Na i,Sii,Cai,Tii and Ti ii,andNii abundances. Stars cooler than ∼5500 show lower Ca i,Tii,andNai than warmer stars. By determining Ti ii abundances, we show that, at least for Ti, this effect is due to NLTE and over-ionization. -
Southern Sky.Pdf
R E A I N S D N I O C I A T T C E E D R I A D L O S S N A G P T M H O E C . H N O O R Z m a r w I i e t h h t I t Z s h t e c i R O g p o e l d O N d t e a n H h C t f l e E I n e o R c i H e t C T a l f L l r o e E D t m s N ( n G NORTH F o A r c O e e M t R H k n T O i E m I a f X N C y A t a . E h Z M s o S i l P E o s P L g e H i SOUTHERN HEMISPHERE E y r A T . A “ N M N E O Capella E Y R W T K T H E S ” B . ) . D O W T E r U i T The Evening Sky Map o W R A n N C DECEMBER 2002 , W . O T T e L l h FREE* EACH MONTH FOR YOU TO EXPLORE, LEARN & ENJOY THE NIGHT SKY H a e E γ E M31 h R H w S AURIGA Algol A u K r n Y S o t T SKY MAP SHOWS HOW r e M C e r E t A , s J P i n s B o A O Sky Calendar – December 2002 t THE NIGHT SKY LOOKS M38 h R m L e O PERSEUS a A U b I e r N s T NE ANDROMEDA i S l EARLY DEC PM D g 10 M37 E a h M36 L c 1 Moon near Venus and Mars at 11h UT (morning sky). -
Science in the Urantia Papers
Science ¾ Scientific Validation of the UB z By Denver Pearson z By Phil Calabrese ¾ Seraphic Velocities ¾ Astronomy The Scientific Integrity of the Urantia Book by Denver Pearson As scientifically minded readers first peruse the Urantia Book, it soon occurs to them that many of its statements on the natural sciences conflict with currently held data and theories. In the minds of many this gives rise to doubts about the truthfulness of those statements. Wisdom would lead us to realize that nothing short of perfection is perfect, and anything touched by human hands has fingerprints. This should be our guiding thoughts as we contemplate the accuracy of the scientific content of the Urantia Papers. Several years ago, at the first scientific symposium, it was implied by one of the speakers that the revelation contains errors. This implication is alarming. More recently, at the second symposium held in Oklahoma, an interesting publication named "The Science Content of The Urantia Book" was made available (this document is obtainable from the Brotherhood of Man Library). In this publication is an article entitled "Time Bombs" in which the author suggests that the revelators planted certain inaccurate scientific statements in the book in order to prevent it from becoming a fetish. He states "...the revelators incorporated safeguards in the papers that would form The Urantia Book to diminish the tendency to regard it as an object of worship. What safeguards did they use? Suppose they decided to make sure that mortals reading it understood that some cosmological statements in the book would be found to be inaccurate". -
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). -
Mid-Infrared Images of Stars and Dust in Irregular Galaxies
Mid-Infrared Images of Stars and Dust in Irregular Galaxies1 Deidre A. Hunter2, Bruce G. Elmegreen3, and Emily Martin2,4 ABSTRACT We present mid-infrared to optical properties of 22 representative irregular galaxies: 18 Im, 3 BCDs, and one Sm. The mid-IR is based on images from the Spitzer Space Telescope archives. The 3.6 and 4.5 µm bands and the UBVJHK images are used to examine disk morphology and the integrated and azimuthally averaged magnitudes and colors of stars. The non-stellar contribution to the 4.5 µm images is used to trace hot dust. The 5.8 and 8.0 µm images reveal emission from hot dust and PAHs, and both may contribute to these passbands, although we refer to the non-stellar emission as PAH emission. We compare the 8.0 µm images to Hα. Im galaxies have no hidden bars, and those with double- exponential optical light profiles have the same at mid-IR. Most galaxies have similar optical and mid-IR scale lengths. Four galaxies have super star clusters that are not visible at optical bands. Galaxies with higher area-normalized star formation rates have more dust and PAH emission relative to starlight. Hot dust and PAH emission is found mostly in high surface brightness H ii regions, implying that massive stars are the primary source of heating. Galaxies with intense, wide-spread star formation have more extended PAH emission. The ratio of PAH to Hα emission is not constant on small scales. PAHs are associated with shells and giant filaments, so they are not destroyed during shell formation. -
And Ecclesiastical Cosmology
GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc.