KLEMOLA Groups and Clusters of Southern Galaxies

Total Page:16

File Type:pdf, Size:1020Kb

KLEMOLA Groups and Clusters of Southern Galaxies KLEMOLA Groups and Clusters of Southern Galaxies Clear Skies Observing Guides - ©V.A. van Wulfen - clearskies.eu - [email protected] Index Klemola 1 (Abell S141) Sculptor Klemola 2 (Abell S301) Fornax Klemola 3 (Vorontsov-Vel'yaminov 1049) Fornax Klemola 4 Fornax Klemola 5 (Abell 3089) Fornax Klemola 6 Horologium Klemola 7 (Abell S339) Horologium Klemola 8 (Abell 3128) Horologium Klemola 9 Caelum Klemola 10 Puppis Klemola 11 Antlia Klemola 12 Vela Klemola 13 Hydra Klemola 14 Vela Klemola 15 (Abell S639) Vela Klemola 16 Antlia Klemola 17 (Abell S649) Hydra Klemola 18 Centaurus Klemola 19 Centaurus Klemola 20 (Abell 3526) - "Centaurus Cluster" Centaurus Klemola 21 (Abell 3528) Hydra Klemola 22 (Abell 3532) Centaurus Klemola 23 Centaurus Klemola 24 Centaurus Klemola 25 (Abell S734) Centaurus Klemola 26 Hydra Klemola 27 (Abell 3574) Centaurus Klemola 28 Hydra Klemola 29 Centaurus Klemola 30 (Rose 38) - "NGC6845 Quartet" Telescopium Klemola 31 Sagittarius Klemola 32 (Abell S947) Grus Klemola 33 (Abell S974) Grus Klemola 34 (Hickson 90) Piscis Austrinus Klemola 35 Aquarius Klemola 36 Piscis Austrinus Klemola 37 Piscis Austrinus Klemola 38 (Abell S997) Piscis Austrinus Klemola 39 Piscis Austrinus Klemola 40 (Hickson 91) Piscis Austrinus Klemola 41 (Abell S1005) Grus Klemola 42 Piscis Austrinus Klemola 43 (Abell 2511) Aquarius Klemola 44 (Abell 4038) Sculptor Klemola Groups and Clusters of Southern Galaxies 2 V2.4 Clear Skies Observing Guides - ©V.A. van Wulfen - clearskies.eu - [email protected] Index - by constellation ANTLIA Klemola 11 Klemola 16 AQUARIUS Klemola 35 Klemola 43 (Abell 2511) CAELUM Klemola 9 CENTAURUS Klemola 18 Klemola 19 Klemola 20 (Abell 3526) - "Centaurus Cluster" Klemola 22 (Abell 3532) Klemola 23 Klemola 24 Klemola 25 (Abell S734) Klemola 27 (Abell 3574) Klemola 29 FORNAX Klemola 2 (Abell S301) Klemola 4 Klemola 3 (Vorontsov-Vel'yaminov 1049) Klemola 5 GRUS Klemola 32 (Abell S947) Klemola 33 (Abell S974) Klemola 41 (Abell S1005) HOROLOGIUM Klemola 6 Klemola 7 (Abell S339) Klemola 8 (Abell 3128) HYDRA Klemola 13 Klemola 17 (Abell S649) Klemola 21 (Abell 3528) Klemola 26 Klemola 28 PISCIS AUSTRINUS Klemola 34 (Hickson 90) Klemola 36 Klemola 37 Klemola 40 (Hickson 91) Klemola 39 Klemola 38 (Abell S997) Klemola 42 PUPPIS Klemola 10 SAGITTARIUS Klemola 31 SCULPTOR Klemola 44 (Abell 4038) Klemola 1 (Abell S141) TELESCOPIUM Klemola 30 (Rose 38) - "NGC6845 Quartet" VELA Klemola 12 Klemola 14 Klemola 15 (Abell S639) Klemola Groups and Clusters of Southern Galaxies 3 V2.4 Clear Skies Observing Guides - ©V.A. van Wulfen - clearskies.eu - [email protected] .
Recommended publications
  • Where Are the Distant Worlds? Star Maps
    W here Are the Distant Worlds? Star Maps Abo ut the Activity Whe re are the distant worlds in the night sky? Use a star map to find constellations and to identify stars with extrasolar planets. (Northern Hemisphere only, naked eye) Topics Covered • How to find Constellations • Where we have found planets around other stars Participants Adults, teens, families with children 8 years and up If a school/youth group, 10 years and older 1 to 4 participants per map Materials Needed Location and Timing • Current month's Star Map for the Use this activity at a star party on a public (included) dark, clear night. Timing depends only • At least one set Planetary on how long you want to observe. Postcards with Key (included) • A small (red) flashlight • (Optional) Print list of Visible Stars with Planets (included) Included in This Packet Page Detailed Activity Description 2 Helpful Hints 4 Background Information 5 Planetary Postcards 7 Key Planetary Postcards 9 Star Maps 20 Visible Stars With Planets 33 © 2008 Astronomical Society of the Pacific www.astrosociety.org Copies for educational purposes are permitted. Additional astronomy activities can be found here: http://nightsky.jpl.nasa.gov Detailed Activity Description Leader’s Role Participants’ Roles (Anticipated) Introduction: To Ask: Who has heard that scientists have found planets around stars other than our own Sun? How many of these stars might you think have been found? Anyone ever see a star that has planets around it? (our own Sun, some may know of other stars) We can’t see the planets around other stars, but we can see the star.
    [Show full text]
  • Chemistry and Kinematics of Stars in Local Group Galaxies
    Chemistry and kinematics of stars in Local Group galaxies Giuseppina Battaglia ESO Garching In collaboration with DART (E.Tolstoy, M.Irwin, A.Helmi, V.Hill, B.Letarte, P.Jablonka, K.Venn, M.Shetrone, N.Arimoto, F.Primas, A.Kaufer, T. Szeifert, P. François,T.Abel) Dwarf spheroidal galaxies Small (half-light radius= 0.1-1kpc), devoid of gas, pressure supported SSccuulplpttoorr FFoorrnnaaxx Typical dSph Unusual dSph • Distance: 79 kpc • Distance: 138 kpc • Faint (Lv~ 10^6 Lsun) • Most luminous (Lv~10^7 Lsun) and and metal poor metal rich of MW satellites SFHs from Grebel, Gallagher & Harbeck 2007 (see also Monkiewicz et al. 1999, Stetson et al. 1998, Buonanno et al.1999, Saviane et al. 2000) Time [Gyr] Time [Gyr] Motivation • Galaxy formation on the smallest scales – Evolution and distribution of stellar populations – Chemical enrichment histories – All dSphs contain > 10 Gyr old stars => early universe • Most dark-matter dominated galaxies – Measure dark-matter distribution – Constrain the nature of dark-matter (warm, cold...) • Galaxy formation: building blocks of large galaxies? TThhee LLooccaall GGrroouupp Grebel et al. 2000 Large Dwarf ellipticals (dE); Dwarf irregulars dSphs/dIrrs spirals dwarf spheroidals (dSphs) (dIrr) dI rr Large majority DDAARRTT LLaarrggee PPrrooggrraamm aatt EESSOO • 4 dSphs in the MW halo: Sextans, Sculptor, Fornax, Carina (HR only) • Extended ESO/WFI imaging (CMD) probable members • VLT/FLAMES Low Resolution (LR) X probable non members spectra of 100s Red Giant Branch (RGB) stars in CaII triplet (CaT) region
    [Show full text]
  • Tip of the Red Giant Branch Distance for the Sculptor Group Dwarf ESO 540-032?
    A&A 371, 487–496 (2001) Astronomy DOI: 10.1051/0004-6361:20010389 & c ESO 2001 Astrophysics Tip of the red giant branch distance for the Sculptor group dwarf ESO 540-032? H. Jerjen1 and M. Rejkuba2,3 1 Research School of Astronomy and Astrophysics, The Australian National University, Mt Stromlo Observatory, Cotter Road, Weston ACT 2611, Australia 2 European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei M¨unchen, Germany e-mail: [email protected] 3 Department of Astronomy, P. Universidad Cat´olica, Casilla 306, Santiago 22, Chile Received 19 January 2001 / Accepted 9 March 2001 Abstract. We present the first VI CCD photometry for the Sculptor group galaxy ESO 540-032 obtained at the Very Large Telescope UT1+FORS1. The (I, V − I) colour-magnitude diagram indicates that this intermediate- type dwarf galaxy is dominated by old, metal-poor ([Fe/H] ≈−1.7 dex) stars, with a small population of slightly more metal-rich ([Fe/H] ≈−1.3 dex), young (age 150 − 500 Myr) stars. A discontinuity in the I-band luminosity function is detected at I0 =23.44 0.09 mag. Interpreting this feature as the tip of the red giant branch and adopting MI = −4.20 0.10 mag for its absolute magnitude, we have determined a Population II distance modulus of (m − M)0 =27.64 0.14 mag (3.4 0.2 Mpc). This distance confirms ESO 540-032 as a member of the nearby Sculptor group but is significantly larger than a previously reported value based on the Surface Brightness Fluctuation (SBF) method.
    [Show full text]
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • The Lore of the Stars, for Amateur Campfire Sages
    obscure. Various claims have been made about Babylonian innovations and the similarity between the Greek zodiac and the stories, dating from the third millennium BCE, of Gilgamesh, a legendary Sumerian hero who encountered animals and characters similar to those of the zodiac. Some of the Babylonian constellations may have been popularized in the Greek world through the conquest of The Lore of the Stars, Alexander in the fourth century BCE. Alexander himself sent captured Babylonian texts back For Amateur Campfire Sages to Greece for his tutor Aristotle to interpret. Even earlier than this, Babylonian astronomy by Anders Hove would have been familiar to the Persians, who July 2002 occupied Greece several centuries before Alexander’s day. Although we may properly credit the Greeks with completing the Babylonian work, it is clear that the Babylonians did develop some of the symbols and constellations later adopted by the Greeks for their zodiac. Contrary to the story of the star-counter in Le Petit Prince, there aren’t unnumerable stars Cuneiform tablets using symbols similar to in the night sky, at least so far as we can see those used later for constellations may have with our own eyes. Only about a thousand are some relationship to astronomy, or they may visible. Almost all have names or Greek letter not. Far more tantalizing are the various designations as part of constellations that any- cuneiform tablets outlining astronomical one can learn to recognize. observations used by the Babylonians for Modern astronomers have divided the sky tracking the moon and developing a calendar. into 88 constellations, many of them fictitious— One of these is the MUL.APIN, which describes that is, they cover sky area, but contain no vis- the stars along the paths of the moon and ible stars.
    [Show full text]
  • The Constellation Microscopium, the Microscope Microscopium Is A
    The Constellation Microscopium, the Microscope Microscopium is a small constellation in the southern sky, defined in the 18th century by Nicolas Louis de Lacaille in 1751–52 . Its name is Latin for microscope; it was invented by Lacaille to commemorate the compound microscope, i.e. one that uses more than one lens. The first microscope was invented by the two brothers, Hans and Zacharius Jensen, Dutch spectacle makers of Holland in 1590, who were also involved in the invention of the telescope (see below). Lacaille first showed it on his map of 1756 under the name le Microscope but Latinized this to Microscopium on the second edition published in 1763. He described it as consisting of "a tube above a square box". It contains sixty-nine stars, varying in magnitude from 4.8 to 7, the lucida being Gamma Microscopii of apparent magnitude 4.68. Two star systems have been found to have planets, while another has a debris disk. The stars that now comprise Microscopium may formerly have belonged to the hind feet of Sagittarius. However, this is uncertain as, while its stars seem to be referred to by Al-Sufi as having been seen by Ptolemy, Al-Sufi does not specify their exact positions. Microscopium is bordered Capricornus to the north, Piscis Austrinus and Grus to the west, Sagittarius to the east, Indus to the south, and touching on Telescopium to the southeast. The recommended three-letter abbreviation for the constellation, as adopted Seen in the 1824 star chart set Urania's Mirror (lower left) by the International Astronomical Union in 1922, is 'Mic'.
    [Show full text]
  • Sydney Observatory Night Sky Map September 2012 a Map for Each Month of the Year, to Help You Learn About the Night Sky
    Sydney Observatory night sky map September 2012 A map for each month of the year, to help you learn about the night sky www.sydneyobservatory.com This star chart shows the stars and constellations visible in the night sky for Sydney, Melbourne, Brisbane, Canberra, Hobart, Adelaide and Perth for September 2012 at about 7:30 pm (local standard time). For Darwin and similar locations the chart will still apply, but some stars will be lost off the southern edge while extra stars will be visible to the north. Stars down to a brightness or magnitude limit of 4.5 are shown. To use this chart, rotate it so that the direction you are facing (north, south, east or west) is shown at the bottom. The centre of the chart represents the point directly above your head, called the zenith, and the outer circular edge represents the horizon. h t r No Star brightness Moon phase Last quarter: 08th Zero or brighter New Moon: 16th 1st magnitude LACERTA nd Deneb First quarter: 23rd 2 CYGNUS Full Moon: 30th rd N 3 E LYRA th Vega W 4 LYRA N CORONA BOREALIS HERCULES BOOTES VULPECULA SAGITTA PEGASUS DELPHINUS Arcturus Altair EQUULEUS SERPENS AQUILA OPHIUCHUS SCUTUM PISCES Moon on 23rd SERPENS Zubeneschamali AQUARIUS CAPRICORNUS E SAGITTARIUS LIBRA a Saturn Centre of the Galaxy Antares Zubenelgenubi t s Antares VIRGO s t SAGITTARIUS P SCORPIUS P e PISCESMICROSCOPIUM AUSTRINUS SCORPIUS Mars Spica W PISCIS AUSTRINUS CORONA AUSTRALIS Fomalhaut Centre of the Galaxy TELESCOPIUM LUPUS ARA GRUSGRUS INDUS NORMA CORVUS INDUS CETUS SCULPTOR PAVO CIRCINUS CENTAURUS TRIANGULUM
    [Show full text]
  • ANIRUDH CHITI [email protected]
    ANIRUDH CHITI [email protected] Education & Appointments Kavli Institute for Cosmological Physics, University of Chicago Sep 2021 { Present Brinson Prize Fellow in Observational Astrophysics Massachusetts Institute of Technology May 2021 Ph.D. in Physics Advised by Anna Frebel Cornell University May 2014 B.A. in Physics Magna Cum Laude and B.A. in Mathematics with Distinction Minor in Astronomy Awards & Honors Henry Kendall Teaching Award, Graduate teaching award in Physics 2016 Honorable Mention, NSF Graduate Research Fellowship Program 2016 Whiteman Fellow, First-year fellowship at MIT 2014 { 2015 Cranston and Edna Shelley Award, Undergraduate research award in Astronomy 2014 Dean's List, Cornell University, GPA-based award Fall 2010 { Fall 2013 Competitively Obtained Telescope Time PI, 6 nights on Magellan/IMACS { Imaging (2020A, 2020B) PI, 8 nights on Magellan/IMACS { Multi-slit spectroscopy (2015B, 2016A, 2016B, 2018A) PI, 12 nights on Magellan/MagE { Single-slit spectroscopy, (2016B, 2018A, 2018B, 2019A, 2019B) PI, 1 night on Magellan/M2FS { Multi-fiber spectroscopy, (2016A) PI, 1.5 nights on Magellan/MIKE { Single-slit spectroscopy, (2020B) Co-I, 2 nights on Magellan/M2FS { Multi-fiber spectroscopy, (2015A) Co-I, 6 nights on Magellan/MIKE { Single-slit spectroscopy, (2016B, 2019A) Co-I, 30 hours on SkyMapper { Imaging, (2017B, 2018A) Professional Service & Leadership Experience Referee for ApJ, MNRAS, PASJ 2019 { Present Research Advisor for MIT undergraduates: Kylie Hansen May 2019 { May 2020 Tatsuya Daniel Aug 2019 { May 2020 Organizing Committee, JINA-CEE Frontiers in Nuclear Astrophysics Meeting May 2018 Co-director & Founding member, MIT Sidewalk Astronomy Club Fall 2017 { Aug 2020 Organized 10+ sidewalk stargazing sessions, serving over 400 members of the public in total Online Project Course Instructor, MIT MOSTEC Summers 2015 { 2018 Instructed an online astrophysics course for rising seniors in high school.
    [Show full text]
  • Horologium II: a Second Ultra-Faint Milky Way Satellite in the Horologium Constellation
    Draft version August 21, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 HOROLOGIUM II: A SECOND ULTRA-FAINT MILKY WAY SATELLITE IN THE HOROLOGIUM CONSTELLATION Dongwon Kim and Helmut Jerjen Research School of Astronomy and Astrophysics, The Australian National University, Mt Stromlo Observatory, via Cotter Rd, Weston, ACT 2611, Australia Draft version August 21, 2018 ABSTRACT We report the discovery of a new ultra-faint Milky Way satellite candidate, Horologium II, detected in the Dark Energy Survey Y1A1 public data. Horologium II features a half light radius of rh = +0:2 47 ± 10 pc and a total luminosity of MV = −2:6−0:3 that place it in the realm of ultra-faint dwarf galaxies on the size-luminosity plane. The stellar population of the new satellite is consistent with an old (∼ 13:5 Gyr) and metal-poor ([Fe/H]∼ −2:1) isochrone at a distance modulus of (m − M) = 19:46 ± 0:20, or a heliocentric distance of 78 ± 8 kpc, in the color-magnitude diagram. Horologium II has a distance similar to the Sculptor dwarf spheroidal galaxy (∼ 82 kpc) and the recently reported ultra-faint satellites Eridanus III (87±8 kpc) and Horologium I (79±8 kpc). All four satellites are well aligned on the sky, which suggests a possible common origin. As Sculptor is moving on a retrograde orbit within the Vast Polar Structure when compared to the other classical MW satellite galaxies including the Magellanic Clouds, this hypothesis can be tested once proper motion measurements become available. Subject headings: Local Group - Galaxy: halo - galaxies: dwarf - galaxies: individual (Horologium II) - galaxies: stellar content 1.
    [Show full text]
  • Population Gradients in Local Group Dwarf Spheroidals
    Population Gradients in Local Group Dwarf Spheroidals Daniel Harbeck1, Eva K. Grebel1,11, Jon Holtzman2, Puragra Guhathakurta3, Wolfgang Brandner4,5, Doug Geisler6,11 , Ata Sarajedini7,11, Andrew Dolphin8, Denise Hurley-Keller9,10,11, Mario Mateo10,11 ABSTRACT We present a systematic and homogeneous analysis of population gradients for the Local Group dwarf spheroidals (dSphs) Carina, Sculptor, Sextans, Tucana, Andromeda I-III, V, and VI. For all of the Milky Way companions studied here we find significant population gradients. The same is true for the remote dSph Tucana located at the outskirts of the LG. Among the M 31 dSph companions only Andromeda I and VI show obvious gradients. In all cases where a HB morphology gradient is visible, the red HB stars are more centrally concentrated. The occurence of a HB morphological gradient shows a correlation with a morphology gradient in the red giant branch. It seems likely that metallicity is the driver of the gradients in Sextans, Sculptor, Tucana, and Andromeda VI, while age is an important factor in Carina. We find no evidence that the vicinity of a nearby massive spiral galaxy influences the formation of the population gradients. Subject headings: galaxies: dwarf – galaxies: structure – galaxies: stellar content – stars: abundances – stars: horizontal-branch – Local Group 1Max-Planck-Institut f¨ur Astronomie, K¨onigstuhl 17, D-69117 Heidelberg, Germany 2New Mexico State University, Department 4500, Box 30001, Las Cruces, NM 88003 arXiv:astro-ph/0109121v1 7 Sep 2001 3UCO/Lick Observatory, University of California at Santa Cruz, Santa Cruz, CA 95064, USA 4University of Hawaii, Institute for Astronomy, 2680 Woodlawn Dr., Honolulu, HI 96822 5European Southern Observatory, Karl-Schwarzschild-Str.
    [Show full text]
  • These Sky Maps Were Made Using the Freeware UNIX Program "Starchart", from Alan Paeth and Craig Counterman, with Some Postprocessing by Stuart Levy
    These sky maps were made using the freeware UNIX program "starchart", from Alan Paeth and Craig Counterman, with some postprocessing by Stuart Levy. You’re free to use them however you wish. There are five equatorial maps: three covering the equatorial strip from declination −60 to +60 degrees, corresponding roughly to the evening sky in northern winter (eq1), spring (eq2), and summer/autumn (eq3), plus maps covering the north and south polar areas to declination about +/− 25 degrees. Grid lines are drawn at every 15 degrees of declination, and every hour (= 15 degrees at the equator) of right ascension. The equatorial−strip maps use a simple rectangular projection; this shows constellations near the equator with their true shape, but those at declination +/− 30 degrees are stretched horizontally by about 15%, and those at the extreme 60−degree edge are plotted twice as wide as you’ll see them on the sky. The sinusoidal curve spanning the equatorial strip is, of course, the Ecliptic −− the path of the Sun (and approximately that of the planets) through the sky. The polar maps are plotted with stereographic projection. This preserves shapes of small constellations, but enlarges them as they get farther from the pole; at declination 45 degrees they’re about 17% oversized, and at the extreme 25−degree edge about 40% too large. These charts plot stars down to magnitude 5, along with a few of the brighter deep−sky objects −− mostly star clusters and nebulae. Many stars are labelled with their Bayer Greek−letter names. Also here are similarly−plotted maps, based on galactic coordinates.
    [Show full text]
  • Model Comparison of the Dark Matter Profiles
    A&A 558, A35 (2013) Astronomy DOI: 10.1051/0004-6361/201321606 & c ESO 2013 Astrophysics Model comparison of the dark matter profiles of Fornax, Sculptor, Carina and Sextans Maarten A. Breddels and Amina Helmi Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands e-mail: [email protected] Received 28 March 2013 / Accepted 16 August 2013 ABSTRACT Aims. We compare dark matter profile models of four dwarf spheroidal galaxies satellites of the Milky Way using Bayesian evidence. Methods. We use orbit based dynamical models to fit the 2nd and 4th moments of the line of sight velocity distributions of the Fornax, Sculptor, Carina and Sextans dwarf spheroidal galaxies. We compare NFW, Einasto and several cored profiles for their dark halos and present the probability distribution functions of the model parameters. Results. For each galaxy separately we compare the evidence for the various dark matter profiles, and find that it is not possible to distinguish between these specific parametric dark matter density profiles using the current data. Nonetheless, from the combined 2 β/2 evidence, we find that is unlikely that all galaxies are embedded in the same type of cored profiles of the form ρDM ∝ 1/(1 + r ) , where β = 3, 4. For each galaxy, we also obtain an almost model independent, and therefore accurate, constraint on the logarithmic slope of the dark matter density distribution at a radius ∼r−3, i.e. where the logarithmic slope of the stellar density profile is −3. Conclusions. For each galaxy, we find that all best fit models essentially have the same mass distribution over a large range in radius (from just below r−3 to the last measured data point).
    [Show full text]