Herschel 2500 Observing Logbook!

Total Page:16

File Type:pdf, Size:1020Kb

Herschel 2500 Observing Logbook! The Herschel – 2500 William and Caroline Herschel 1 William Herschel published his deep-sky discoveries as three separate catalogues: Catalogue of One Thousand New Nebulae and Clusters of Stars (1786), Catalogue of a Second Thousand New Nebulae and Clusters of Stars (1789), Catalogue of 500 New Nebulae ... (1802). Herschel classified his list into eight sub-categories: Class I - Bright Nebulae; Class II - Faint Nebulae; Class III - Very Faint Nebulae; Class IV - Planetary Nebulae; Class V - Very Large Nebulae; Class VI - Very Compressed and Rich Clusters of Stars; Class VII - Compressed Clusters of Small and Large Stars; Class VIII - Coarsely Scattered Clusters of Stars. Class I - Bright Nebulae: This Herschel class tends to be objects of various sizes and shapes, such as galaxies, clusters, and nebula. But the one thing they all have in common is that they are very bright. These are the easiest Herschel Objects to observe. Class II - Faint Nebulae: This Herschel class tends to be objects that are generally faint, such as unresolved clusters and dim galaxies. You’ll need fairly dark skies and a medium to large telescope. Class III - Very Faint Nebulae: This Herschel class tends to be made up of very, very faint objects, mostly galaxies. This class of objects will require a dark sky location, a large telescope, or video / CCD camera, and a bit of luck. Class IV - Planetary Nebulae: This Herschel class tends to be made up of objects that are actually planetary nebula, but you can find some emission nebula and galaxies mixed in. Class V - Very Large Nebulae: This Herschel class tends to consist of very large deep-sky objects. They may not necessarily be very bright. Depending on the object, you may need a dark-sky location, and a wide-field eyepiece. Class VI - Very Compressed and Rich Clusters of Stars: This Herschel class tends to be mostly bright resolvable globular clusters, and large open clusters with numerous members. Class VII - Compressed Clusters of Small and Large Stars: This Herschel class tends to be open clusters containing bright fore-ground stars, or cluster members with widely varying luminosities. Class VIII - Coarsely Scattered Clusters of Stars: This Herschel class tends to be loose, somewhat dim open clusters. Best suited for wide-field eyepieces. Actually only 2482 total objects 2 Name Con Herschel# Type Mag Size R. A. Dec Notes Date NGC 13 And H866-3 Galaxy 13.6 2.7 00:08.8 +33~26 NGC 29 And H853-2 Galaxy 12.6 1.8 00:10.8 +33~21 NGC 39 And H861-3 Galaxy 13.5 1.1 00:12.3 +31~03 NGC 68 And H16-5 Galaxy 13 1.5 00:18.3 +30~04 NGC 108 And H148-3 Galaxy 12.1 2.3 00:25.9 +29~13 NGC 160 And H476-3 Galaxy 12.4 3.2 00:36.1 +23~57 "400" M110 M31 NGC 205 And H18-5 Galaxy 8 17.4 00:40.4 +41~41 group Knot in NGC 206 And H36-5 4.2 00:40.6 +40~44 with M31 galaxy NGC 214 And H209-2 Galaxy 12.2 2.1 00:41.5 +25~30 NGC 233 And H149-3 Galaxy 12.4 2 00:43.4 +30~35 Brightest in NGC 252 And H609-2 Galaxy 12.3 1.7 00:48.0 +27~38 group NGC 280 And H477-3 Galaxy 13.2 1.6 00:52.5 +24~20 distorted NGC 393 And H54-1 Galaxy 12.5 1.7 01:08.6 +39~40 "400" Near Beta NGC 404 And H224-2 Galaxy 10.1 4.4 01:09.4 +35~43 And NGC 477 And H577-3 Galaxy 13 2.3 01:21.3 +40~29 main arms split NGC 513 And H169-3 Galaxy 12.9 0.7 01:23.8 +33~49 NGC 523 And H170-3 Galaxy 12.7 2.9 01:25.3 +34~02 Peculiar SAC?* NGC 536 And H171-3 Galaxy 12.3 3.1 01:26.4 +34~43 NGC 537 And H170-3 Nonexistent 01:26.3 +34~05 NGC 551 And H560-3 Galaxy 12.7 1.8 01:27.6 +37~11 NGC 679 And H175-3 Galaxy 12.4 2.3 01:49.7 +35~47 NGC 687 And H561-3 Galaxy 12.3 1.4 01:50.6 +36~21 NGC 703 And H562-3 Galaxy 13.3 1.2 01:52.8 +36~09 NGC 708 group NGC 704 And H563-3 Galaxy 13.1 01:52.7 +36~06 Double system NGC 705 And H564-3 Galaxy 13.6 1.1 01:52.8 +36~08 NGC 708 group NGC 708 And H565-3 Galaxy 12.7 3 01:52.8 +36~10 NGC 708 group Open NGC 752 And H32-7 5.7 50 01:57.8 +37~41 "400" 70 stars cluster NGC 797 And H566-3 Galaxy 12.2 1.7 02:03.4 +38~07 double nebula NGC 818 And H604-2 Galaxy 12.5 3.2 02:08.7 +38~47 NGC 828 And H605-2 Galaxy 12.2 3.2 02:10.2 +39~12 Peculiar NGC 834 And H567-3 Galaxy 13.1 1.1 02:11.0 +37~40 NGC 845 And H604-3 Galaxy 13.5 1.6 02:12.3 +37~29 "400" NGC 1023 NGC 891 And H19-5 Galaxy 10 13.5 02:22.6 +42~21 group NGC 898 And H570-3 Galaxy 12.9 1.8 02:23.3 +41~57 NGC 910 And H571-3 Galaxy 12.2 2.2 02:25.4 +41~50 NGC 980 And H572-3 Galaxy 13 1.7 02:35.5 +40~54 NGC 982 And H573-3 Galaxy 12.5 1.6 02:35.4 +40~57 NGC 7640 And H600-2 Galaxy 10.9 10.7 23:22.1 +40~51 nearly edge on Planetary "400" Blue NGC 7662 And H18-4 8.3 0.1 23:25.9 +42~33 Neb Snowball Open NGC 7686 And H69-8 5.6 14 23:30.2 +49~08 "400" cluster NGC 7707 And H579-3 Galaxy 13.4 1.2 23:34.8 +44~18 NGC 2997 Ant H50-5 Galaxy 9.3 10 09:45.6 -31~11 NGC 6728 Aql H13-8 Nonexistent 19:00.0 - 8~57 Open NGC 6755 Aql H19-7 7.5 15 19:07.8 + 4~14 "400" cluster 3 Name Con Herschel# Type Mag Size R. A. Dec Notes Date Open NGC 6756 Aql H62-7 10.6 4 19:08.7 + 4~41 "400" cluster Planetary NGC 6772 Aql H14-4 14.2 1 19:14.6 - 2~42 Neb Planetary NGC 6781 Aql H743-3 11.4 1.8 19:18.4 + 6~33 "400" Neb Planetary NGC 6804 Aql H38-6 12 1.1 19:31.6 + 9~13 Neb NGC 6814 Aql H744-3 Galaxy 11.2 3.2 19:42.7 -10~19 NGC 6828 Aql H73-8 Nonexistent 19:50.4 + 7~55 Open Not in NGC 6837 Aql H18-8 19:53.5 +11~41 cluster Uranometria Open Not in NGC 6840 Aql H19-8 19:55.3 +12~06 cluster Uranometria NGC 6926 Aql H142-3 Galaxy 12.4 2.1 20:33.1 - 2~01 with NGC 6962 Aqr H426-2 Galaxy 12 3 20:47.3 + 0~19 6959,61,63,64,67 with NGC 6964 Aqr H427-2 Galaxy 12.7 1.9 20:47.4 + 0~18 6959,61,62,63,67 Planetary "400" Saturn NGC 7009 Aqr H1-4 8.3 1.7 21:04.2 -11~22 Neb Nebula NGC 7081 Aqr H859-3 Galaxy 12.7 1 21:31.4 + 2~30 NGC 7165 Aqr H930-3 Galaxy 13.5 1 21:59.5 -16~31 NGC 7171 Aqr H692-3 Galaxy 12.2 2.1 22:01.0 -13~16 NGC 7180 Aqr H693-3 Galaxy 12.5 1.8 22:02.3 -20~33 NGC 7183 Aqr H595-2 Galaxy 11.9 4.1 22:02.4 -18~56 NGC 7184 Aqr H1-2 Galaxy 11.2 6.5 22:02.7 -20~49 NGC 7218 Aqr H897-2 Galaxy 12 2.8 22:10.2 -16~40 NGC 7230 Aqr H931-3 Galaxy 13.5 1.1 22:14.3 -17~04 NGC 7246 Aqr H932-3 Galaxy 14.6 1.8 22:17.5 -15~32 NGC 7251 Aqr H933-3 Galaxy 11.8 1.8 22:20.4 -15~46 NGC 7252 Aqr H458-3 Galaxy 12.1 2.2 22:20.7 -24~41 NGC 7284 Aqr H469-2 Galaxy 11.9 2.2 22:28.6 -24~51 NGC 7302 Aqr H31-4 Galaxy 12.2 2.1 22:32.4 -14~07 NGC 7309 Aqr H476-2 Galaxy 12.5 1.6 22:34.3 -10~21 NGC 7364 Aqr H442-2 Galaxy 12.6 1.6 22:44.5 - 0~07 NGC 7371 Aqr H477-2 Galaxy 12.1 2.1 22:46.1 -11~00 Faint outer ring NGC 7377 Aqr H598-2 Galaxy 11.6 2.2 22:47.8 -22~19 NGC 7391 Aqr H443-2 Galaxy 12 1.8 22:50.7 - 1~31 NGC 7392 Aqr H702-2 Galaxy 11.9 2 22:51.8 -20~36 NGC 7393 Aqr H453-2 Galaxy 12.6 2 22:51.7 - 5~33 NGC 7443 Aqr H450-2 Galaxy 12.6 1.5 23:00.1 -12~48 with NGC7444 NGC 7444 Aqr H451-2 Galaxy 12.8 1.4 23:00.1 -12~50 with NGC7443 NGC 7492 Aqr H558-3 Globular 11.5 6.2 23:08.4 -15~37 NGC 7526 Aqr H470-3 Asterism 23:13.9 - 9~12 NGC 7576 Aqr H454-2 Galaxy 13 1.5 23:17.4 - 4~44 NGC 7585 Aqr H236-2 Galaxy 11.7 2.3 23:18.0 - 4~39 NGC 7592 Aqr H186-3 Galaxy 14.2 1.1 23:18.4 - 4~25 colliding pair NGC 7600 Aqr H431-2 Galaxy 11.9 3 23:18.9 - 7~35 NGC 7606 Aqr H104-1 Galaxy 10.8 5.8 23:19.1 - 8~29 "400" NGC 7665 Aqr H438-3 Galaxy 12.7 0.9 23:27.2 - 9~24 NGC 7721 Aqr H432-2 Galaxy 11.6 3.3 23:38.8 - 6~31 4 Name Con Herschel# Type Mag Size R.
Recommended publications
  • John J. Cowan Date of Birth: April 3, 1948 Place of Birth: Washington, D.C
    VITA NAME: John J. Cowan Date of Birth: April 3, 1948 Place of Birth: Washington, D.C. EDUCATION: 1970 B.A. George Washington University, Washington, D.C. 1972 M.S. Case Institute of Technology, Cleveland, OH 1976 Ph.D. University of Maryland, College Park, MD PROFESSIONAL EXPERIENCE: 2002–present David Ross Boyd Professor, University of Oklahoma, 2002–2002 Research Fellow, University of Texas, Austin, TX 1998–2002 Samuel Roberts Noble Foundation Presidential Professor, University of Oklahoma, Norman, OK 1997–1998 Big XIIFaculty Fellow,University ofOklahoma 1991–1992 Visiting Professor, Department of Astronomy, Columbia University, New York, NY 1989–present Professor, Department of Physics and Astronomy, University of Oklahoma, Norman, OK 1988–1994 Consultant and Participating Guest, Lawrence Livermore National Laboratory, Livermore, CA 1987–1988 Visiting Research Associate, Harvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 1984–1989 Associate Professor, University of Oklahoma 1979–1984 Assistant Professor, University of Oklahoma 1976–1979 Postdoctoral Research Fellow, Harvard-Smithsonian Center for Astrophysics, Harvard University PROFESSIONAL AND HONORARY SOCIETIES: American Astronomical Society International Astronomical Union Phi Beta Kappa RESEARCH INTERESTS: Stellar evolution, supernovae, nucleosynthesis and abundances Radio observations of supernovae and galaxies JOHN J. COWAN Page 2 PUBLICATIONS J. J. Cowan and W. K. Rose, “Production of 17O and 18O by Means of the Hot CNO Tri-Cycle,” Astrophys. J. (Letters) 201, L45 (1975) J. J. Cowan, M. Kafatos, and W. K. Rose, “Sources of Excitation of the Interstellar Gas and Galactic Structure,” Astrophys. J. 195, 47 (1975) M. F. A’Hearn and J. J. Cowan, “Molecular Production Rates in Comet Kohoutek,” As- tron.
    [Show full text]
  • Infrared Spectroscopy of Nearby Radio Active Elliptical Galaxies
    The Astrophysical Journal Supplement Series, 203:14 (11pp), 2012 November doi:10.1088/0067-0049/203/1/14 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. INFRARED SPECTROSCOPY OF NEARBY RADIO ACTIVE ELLIPTICAL GALAXIES Jeremy Mould1,2,9, Tristan Reynolds3, Tony Readhead4, David Floyd5, Buell Jannuzi6, Garret Cotter7, Laura Ferrarese8, Keith Matthews4, David Atlee6, and Michael Brown5 1 Centre for Astrophysics and Supercomputing Swinburne University, Hawthorn, Vic 3122, Australia; [email protected] 2 ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) 3 School of Physics, University of Melbourne, Melbourne, Vic 3100, Australia 4 Palomar Observatory, California Institute of Technology 249-17, Pasadena, CA 91125 5 School of Physics, Monash University, Clayton, Vic 3800, Australia 6 Steward Observatory, University of Arizona (formerly at NOAO), Tucson, AZ 85719 7 Department of Physics, University of Oxford, Denys, Oxford, Keble Road, OX13RH, UK 8 Herzberg Institute of Astrophysics Herzberg, Saanich Road, Victoria V8X4M6, Canada Received 2012 June 6; accepted 2012 September 26; published 2012 November 1 ABSTRACT In preparation for a study of their circumnuclear gas we have surveyed 60% of a complete sample of elliptical galaxies within 75 Mpc that are radio sources. Some 20% of our nuclear spectra have infrared emission lines, mostly Paschen lines, Brackett γ , and [Fe ii]. We consider the influence of radio power and black hole mass in relation to the spectra. Access to the spectra is provided here as a community resource. Key words: galaxies: elliptical and lenticular, cD – galaxies: nuclei – infrared: general – radio continuum: galaxies ∼ 1. INTRODUCTION 30% of the most massive galaxies are radio continuum sources (e.g., Fabbiano et al.
    [Show full text]
  • CO Multi-Line Imaging of Nearby Galaxies (COMING) IV. Overview Of
    Publ. Astron. Soc. Japan (2018) 00(0), 1–33 1 doi: 10.1093/pasj/xxx000 CO Multi-line Imaging of Nearby Galaxies (COMING) IV. Overview of the Project Kazuo SORAI1, 2, 3, 4, 5, Nario KUNO4, 5, Kazuyuki MURAOKA6, Yusuke MIYAMOTO7, 8, Hiroyuki KANEKO7, Hiroyuki NAKANISHI9 , Naomasa NAKAI4, 5, 10, Kazuki YANAGITANI6 , Takahiro TANAKA4, Yuya SATO4, Dragan SALAK10, Michiko UMEI2 , Kana MOROKUMA-MATSUI7, 8, 11, 12, Naoko MATSUMOTO13, 14, Saeko UENO9, Hsi-An PAN15, Yuto NOMA10, Tsutomu, T. TAKEUCHI16 , Moe YODA16, Mayu KURODA6, Atsushi YASUDA4 , Yoshiyuki YAJIMA2 , Nagisa OI17, Shugo SHIBATA2, Masumichi SETA10, Yoshimasa WATANABE4, 5, 18, Shoichiro KITA4, Ryusei KOMATSUZAKI4 , Ayumi KAJIKAWA2, 3, Yu YASHIMA2, 3, Suchetha COORAY16 , Hiroyuki BAJI6 , Yoko SEGAWA2 , Takami TASHIRO2 , Miho TAKEDA6, Nozomi KISHIDA2 , Takuya HATAKEYAMA4 , Yuto TOMIYASU4 and Chey SAITA9 1Department of Physics, Faculty of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 2Department of Cosmosciences, Graduate School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 3Department of Physics, School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 4Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 5Tomonaga Center for the History of the Universe (TCHoU), University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 6Department of Physical Science, Osaka Prefecture University, Gakuen 1-1,
    [Show full text]
  • A Dissertation Entitled Star Cluster Populations in the Spiral Galaxy
    A Dissertation entitled Star Cluster Populations in the Spiral Galaxy M101 by Lesley A. Simanton Submitted to the Graduate Faculty as partial fulfillment of the requirements for the Doctor of Philosophy Degree in Physics Dr. Rupali Chandar, Committee Chair Dr. John-David Smith, Committee Member Dr. Steven Federman, Committee Member Dr. Bo Gao, Committee Member Dr. Bradley Whitmore, Committee Member Dr. Patricia R. Komuniecki, Dean College of Graduate Studies The University of Toledo August 2015 Copyright 2015, Lesley A. Simanton This document is copyrighted material. Under copyright law, no parts of this document may be reproduced without the expressed permission of the author. An Abstract of Star Cluster Populations in the Spiral Galaxy M101 by Lesley A. Simanton Submitted to the Graduate Faculty as partial fulfillment of the requirements for the Doctor of Philosophy Degree in Physics The University of Toledo August 2015 Most stars form in groups and clusters. Stars clusters range in age from very young (< 3 Myr, embedded in gas clouds) to some of the most ancient objects in the universe (> 13 Gyr), providing clues to the formation and evolution of their host galaxies. Our knowledge of the diversity of star cluster populations has expanded over the last few decades, especially by being able to examine star clusters outside of the Milky Way (MW). In this dissertation, we continue this expansion of extragalactic star cluster studies by examining the star cluster system of the nearby spiral galaxy M101. We utilize photometry from Hubble Space T elescope images to assess luminosity, color, size, and spatial distributions of old star clusters, and spectroscopy from the Gemini- North telescope to determine ages, metallicities, and velocities of a subset of both young and old clusters in M101.
    [Show full text]
  • Messier Plus Marathon Text
    Messier Plus Marathon Object List by Wally Brown & Bob Buckner with additional objects by Mike Roos Object Data - Saguaro Astronomy Club Score is most numbered objects in a single night. Tiebreaker is count of un-numbered objects Observer Name Date Address Marathon Obects __________ Tiebreaker Objects ________ SEQ OBJECT TYPE CON R.A. DEC. RISE TRANSIT SET MAG SIZE NOTES TIME M 53 GLOCL COM 1312.9 +1810 7:21 14:17 21:12 7.7 13.0' NGC 5024, !B,vC,iR,vvmbM,st 12.. NGC 5272, !!,eB,vL,vsmbM,st 11.., Lord Rosse-sev dark 1 M 3 GLOCL CVN 1342.2 +2822 7:11 14:46 22:20 6.3 18.0' marks within 5' of center 2 M 5 GLOCL SER 1518.5 +0205 10:17 16:22 22:27 5.7 23.0' NGC 5904, !!,vB,L,eCM,eRi, st mags 11...;superb cluster M 94 GALXY CVN 1250.9 +4107 5:12 13:55 22:37 8.1 14.4'x12.1' NGC 4736, vB,L,iR,vsvmbM,BN,r NGC 6121, Cl,8 or 10 B* in line,rrr, Look for central bar M 4 GLOCL SCO 1623.6 -2631 12:56 17:27 21:58 5.4 36.0' structure M 80 GLOCL SCO 1617.0 -2258 12:36 17:21 22:06 7.3 10.0' NGC 6093, st 14..., Extremely rich and compressed M 62 GLOCL OPH 1701.2 -3006 13:49 18:05 22:21 6.4 15.0' NGC 6266, vB,L,gmbM,rrr, Asymmetrical M 19 GLOCL OPH 1702.6 -2615 13:34 18:06 22:38 6.8 17.0' NGC 6273, vB,L,R,vCM,rrr, One of the most oblate GC 3 M 107 GLOCL OPH 1632.5 -1303 12:17 17:36 22:55 7.8 13.0' NGC 6171, L,vRi,vmC,R,rrr, H VI 40 M 106 GALXY CVN 1218.9 +4718 3:46 13:23 22:59 8.3 18.6'x7.2' NGC 4258, !,vB,vL,vmE0,sbMBN, H V 43 M 63 GALXY CVN 1315.8 +4201 5:31 14:19 23:08 8.5 12.6'x7.2' NGC 5055, BN, vsvB stell.
    [Show full text]
  • Arxiv:1702.04727V1 [Astro-Ph.GA] 15 Feb 2017 Galaxies at Higher Mass and Luminosity
    Draft version February 17, 2017 Preprint typeset using LATEX style emulateapj v. 12/16/11 THE DRAGONFLY NEARBY GALAXIES SURVEY. III. THE LUMINOSITY FUNCTION OF THE M101 GROUP Shany Danieli1,2,3, Pieter van Dokkum3, Allison Merritt3, Roberto Abraham4,5, Jielai Zhang4,5,6, I. D. Karachentsev7, and L. N. Makarova7 Draft version February 17, 2017 ABSTRACT We obtained follow-up HST observations of the seven low surface brightness galaxies discovered with the Dragonfly Telephoto Array in the field of the massive spiral galaxy M101. Out of the seven galaxies, only three were resolved into stars and are potentially associated with the M101 group at D = 7 Mpc. Based on HST ACS photometry in the broad F606W and F814W filters, we use a maximum likelihood algorithm to locate the Tip of the Red Giant Branch (TRGB) in galaxy color-magnitude diagrams. +0:35 +0:21 +0:25 Distances are 6:38−0:35; 6:87−0:30 and 6:52−0:27 Mpc and we confirm that they are members of the M101 group. Combining the three confirmed low luminosity satellites with previous results for brighter group members, we find the M101 galaxy group to be a sparsely populated galaxy group consisting of seven group members, down to MV = −9:2 mag. We compare the M101 cumulative luminosity function to that of the Milky Way and M31. We find that they are remarkably similar; In fact, the cumulative luminosity function of the M101 group gets even flatter for fainter magnitudes, and we show that the M101 group might exhibit the two known small-scale flaws in the ΛCDM model, namely `the missing satellite' problem and the `too big to fail' problem.
    [Show full text]
  • Winter Constellations
    Winter Constellations *Orion *Canis Major *Monoceros *Canis Minor *Gemini *Auriga *Taurus *Eradinus *Lepus *Monoceros *Cancer *Lynx *Ursa Major *Ursa Minor *Draco *Camelopardalis *Cassiopeia *Cepheus *Andromeda *Perseus *Lacerta *Pegasus *Triangulum *Aries *Pisces *Cetus *Leo (rising) *Hydra (rising) *Canes Venatici (rising) Orion--Myth: Orion, the great ​ ​ hunter. In one myth, Orion boasted he would kill all the wild animals on the earth. But, the earth goddess Gaia, who was the protector of all animals, produced a gigantic scorpion, whose body was so heavily encased that Orion was unable to pierce through the armour, and was himself stung to death. His companion Artemis was greatly saddened and arranged for Orion to be immortalised among the stars. Scorpius, the scorpion, was placed on the opposite side of the sky so that Orion would never be hurt by it again. To this day, Orion is never seen in the sky at the same time as Scorpius. DSO’s ● ***M42 “Orion Nebula” (Neb) with Trapezium A stellar ​ ​ ​ nursery where new stars are being born, perhaps a thousand stars. These are immense clouds of interstellar gas and dust collapse inward to form stars, mainly of ionized hydrogen which gives off the red glow so dominant, and also ionized greenish oxygen gas. The youngest stars may be less than 300,000 years old, even as young as 10,000 years old (compared to the Sun, 4.6 billion years old). 1300 ly. ​ ​ 1 ● *M43--(Neb) “De Marin’s Nebula” The star-forming ​ “comma-shaped” region connected to the Orion Nebula. ● *M78--(Neb) Hard to see. A star-forming region connected to the ​ Orion Nebula.
    [Show full text]
  • Reddening Map and Recent Star Formation in the Magellanic Clouds with the Earlier Studies (E.G., Besla Et Al
    Astronomy & Astrophysics manuscript no. joshi c ESO 2019 June 19, 2019 Reddening map and recent star formation in the Magellanic Clouds based on OGLE IV Cepheids Y. C. Joshi1⋆⋆⋆, A. Panchal1 1Aryabhatta Research Institute of Observational Sciences (ARIES), Manora peak, Nainital 263002, India Received: 05 November 2018; accepted 11 June 2019 Abstract Context. The reddening maps of the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) are constructed using the Cepheid Period-Luminosity (P-L) relations. Aims. We examine reddening distribution across the LMC and SMC through largest data on Classical Cepheids provided by the OGLE Phase IV survey. We also investigate the age and spatio-temporal distributions of Cepheids to understand the recent star formation history in the LMC and SMC. Methods. The V and I band photometric data of 2476 fundamental mode (FU) and 1775 first overtone mode (FO) Cepheids in the LMC and 2753 FU and 1793 FO Cepheids in the SMC are analyzed for their P-L relations. We convert period of FO Cepheids to corresponding period of FU Cepheids before combining the two modes of Cepheids. Both galaxies are divided into small segments and combined FU and FO P-L diagrams are drawn in two bands for each segment. The reddening analysis is performed on 133 segments covering a total area of about 154.6 deg2 in the LMC and 136 segments covering a total area of about 31.3 deg2 in the SMC. By comparing with well calibrated P-L relations of these two galaxies, we determine reddening E(V − I) in each segment and equivalent reddening E(B − V) assuming the normal extinction law.
    [Show full text]
  • The Radio Properties of a Complete Sample of Bright Galaxies
    Aust. J. Phys., 1982,35,321-50 The Radio Properties of a Complete Sample of Bright Galaxies J. I. Harnett School of Physics, University of Sydney, Sydney, N.S.W. 2006. Abstract Results are given for the radio continuum properties of an optically complete sample of 294 bright galaxies, 147 of which have been detected. Data were obtained with the 408 MHz Molonglo Radio Telescope. The radio luminosity functions for all galaxies and for spiral galaxies alone are derived and the radio emission for different galaxy types is investigated. Spectral indices of 73 galaxies which had been detected at other frequencies were derived; the mean index of a reliable subsample is <ex) = -0,71. 1. Introduction There have been many extensive surveys of continuum radio emission from bright galaxies. The earliest comprehensive survey of high sensitivity was that of Cameron (1971a, 1971b) using the Molonglo Cross Radio Telescope at 408 MHz. Cameron observed two optically complete samples south of b = + 18° and defined the radio luminosity function with reasonable statistics at radio powers of ~ 1022 W HZ-I. In the past decade the optical properties of galaxies have been revised so that the selection of an optically complete sample is more reliable. In addition, between 1970 and 1978 the sensitivity of the 408 MHz Molonglo Cross was improved by more than a magnitude, permitting more detections and more accurate measurements of weak' radio emission. Before observations at 408 MHz with the Molonglo Cross ceased in 1978, a new survey was made to improve Cameron's results and provide the best possible data base for subsequent investigations at different frequencies.
    [Show full text]
  • Experiencing Hubble
    PRESCOTT ASTRONOMY CLUB PRESENTS EXPERIENCING HUBBLE John Carter August 7, 2019 GET OUT LOOK UP • When Galaxies Collide https://www.youtube.com/watch?v=HP3x7TgvgR8 • How Hubble Images Get Color https://www.youtube.com/watch? time_continue=3&v=WSG0MnmUsEY Experiencing Hubble Sagittarius Star Cloud 1. 12,000 stars 2. ½ percent of full Moon area. 3. Not one star in the image can be seen by the naked eye. 4. Color of star reflects its surface temperature. Eagle Nebula. M 16 1. Messier 16 is a conspicuous region of active star formation, appearing in the constellation Serpens Cauda. This giant cloud of interstellar gas and dust is commonly known as the Eagle Nebula, and has already created a cluster of young stars. The nebula is also referred to the Star Queen Nebula and as IC 4703; the cluster is NGC 6611. With an overall visual magnitude of 6.4, and an apparent diameter of 7', the Eagle Nebula's star cluster is best seen with low power telescopes. The brightest star in the cluster has an apparent magnitude of +8.24, easily visible with good binoculars. A 4" scope reveals about 20 stars in an uneven background of fainter stars and nebulosity; three nebulous concentrations can be glimpsed under good conditions. Under very good conditions, suggestions of dark obscuring matter can be seen to the north of the cluster. In an 8" telescope at low power, M 16 is an impressive object. The nebula extends much farther out, to a diameter of over 30'. It is filled with dark regions and globules, including a peculiar dark column and a luminous rim around the cluster.
    [Show full text]
  • Rotation Curves of High-Resolution LSB and SPARC Galaxies with Fuzzy and Multistate (Ultralight Boson) Scalar field Dark Matter
    MNRAS 475, 1447–1468 (2018) doi:10.1093/mnras/stx3208 Advance Access publication 2017 December 12 Rotation curves of high-resolution LSB and SPARC galaxies with fuzzy and multistate (ultralight boson) scalar field dark matter T. Bernal,1‹† L. M. Fernandez-Hern´ andez,´ 1 T. Matos2‡ andM.A.Rodr´ıguez-Meza1‡ 1Departamento de F´ısica, Instituto Nacional de Investigaciones Nucleares, AP 18-1027, Ciudad de Mexico´ 11801, Mexico 2Departamento de F´ısica, Centro de Investigacion´ y de Estudios Avanzados del IPN, AP 14-740, Ciudad de Mexico´ 07000, Mexico Accepted 2017 December 8. Received 2017 December 8; in original form 2017 January 4 ABSTRACT Cold dark matter (CDM) has shown to be an excellent candidate for the dark matter (DM) of the Universe at large scales; however, it presents some challenges at the galactic level. The scalar field dark matter (SFDM), also called fuzzy, wave, Bose–Einstein condensate, or ultralight axion DM, is identical to CDM at cosmological scales but different at the galactic ones. SFDM forms core haloes, it has a natural cut-off in its matter power spectrum, and it predicts well-formed galaxies at high redshifts. In this work we reproduce the rotation curves of high- resolution low surface brightness (LSB) and SPARC galaxies with two SFDM profiles: (1) the soliton+NFW profile in the fuzzy DM (FDM) model, arising empirically from cosmological simulations of real, non-interacting scalar field (SF) at zero temperature, and (2) the multistate SFDM (mSFDM) profile, an exact solution to the Einstein–Klein–Gordon equations for a real, self-interacting SF, with finite temperature into the SF potential, introducing several quantum states as a realistic model for an SFDM halo.
    [Show full text]
  • 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).
    [Show full text]