Exploring the Decans

Exploring The Decans Defining A Decan An (Extremely) Brief History Planet, Image and Identity Planetary Rulership Decanic Rulership Method #1: Descending Ptolemaic Order Slowest Aries I Aries II Aries III Taurus I Taurus II Taurus III Gemini I Gemini II Gemini III Mars Sun Venus Mercury Moon Saturn Jupiter Mars Sun Saturn Jupiter Cancer I Cancer II Cancer III Leo I Leo II Leo III Virgo I Virgo II Virgo III Mars Sun Venus Mercury Moon Saturn Jupiter Mars Sun Venus Mercury Venus Libra I Libra II Libra III Scorpio I Scorpio II Scorpio III Sag I Sag II Sag III Mercury Moon Moon Saturn Jupiter Mars Sun Venus Mercury Moon Saturn Cap I Cap II Cap III Aqua I Aqua II Aqua III Pisces I Pisces II Pisces III Fastest Jupiter Mars Sun Venus Mercury Moon Saturn Jupiter Mars Descending Order Inner Wheel Decanic Rulership Method #2: Triplicity Order Examples: Aries I: Aries = Mars Aries II: Leo = Sun Aries III: Sag = Jupiter Leo I: Leo = Sun Leo II: Sag = Jupiter Leo III: Aries = Mars Sag I: Sag = Jupiter Sag II: Aries = Mars Sag III: Leo = Sun Triplicity Order Outer Wheel Dignity By Face Rulership 5 Exaltation 4 Triplicity 3 Bound 2 Face 1 Image Identity The Decans of Aries Aries I: The Axe Mars - Mars Aries II: The Crown Sun – Sun Aries III: A Rose Aflame Venus - Jupiter The Decans of Taurus Aries III: A Rose Aflame Venus - Jupiter Taurus I: The Plow Mercury - Venus Taurus II: Seed and Soil Moon - Mercury Taurus III: A String of Prayer Beads Saturn - Saturn The Decans of Gemini Gemini I: The Apple Jupiter - Mercury Gemini II: The Hermaphrodite Mars - Venus Gemini III: The Executioner’s Blade Sun - Saturn The Decans of Cancer Cancer I: Mother and Child Venus - Moon Cancer II: A Walled Garden Mercury - Mars Cancer III: The Overflowing Cup Moon - Jupiter The Decans of Leo Leo I: The Mask and the Spotlight Saturn - Sun Leo II: A Crown of Laurels Jupiter – Jupiter Leo III: The Banner Mars - Mars The Decans of Virgo Virgo I: The Tree’s Fruit Sun - Mercury Virgo II: The Hammer and Anvil Venus - Saturn Virgo III: The Sarcophagus Mercury - Venus The Decans of Libra Libra I: The Sword and the Blindfold Moon - Venus Libra II: Links of a Chain Saturn – Saturn Libra III: The Gyroscope Jupiter - Mercury The Decans of Scorpio Scorpio I: The Jaw Bone Mars - Mars Scorpio II: Dual Distillation Sun - Jupiter Scorpio III: A Crow Venus - Moon The Decans of Sagittarius Sagittarius I: The Poisoned Arrow Mercury - Jupiter Sagittarius II: A Bridle Moon – Mars Sagittarius III: A Horse Skull Saturn - Sun The Decans of Capricorn Capricorn I: A Headless Man Jupiter - Saturn Capricorn II: A Pyramid Mars - Venus Capricorn III: The Throne Sun - Mercury The Decans of Aquarius Talk- Decans History Worskhop Aquarius I: The Mark of Exile A Tour of the Decans 5 hours = 300 minutes 15 min/sign Venus - Saturn Aquarius II: Heaven and Earth Mercury – Mercury Aquarius III: The Knot Moon - Venus The Decans of Pisces Pisces I: The Labyrinth Saturn - Jupiter Pisces II: The Net Jupiter - Moon Pisces III: A Bowl of Blood Mars - Mars .

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Distribution of Phantom Dark Matter in Dwarf Spheroidals Alistair O
A&A 640, A26 (2020) Astronomy https://doi.org/10.1051/0004-6361/202037634 & c ESO 2020 Astrophysics Distribution of phantom dark matter in dwarf spheroidals Alistair O. Hodson1,2, Antonaldo Diaferio1,2, and Luisa Ostorero1,2 1 Dipartimento di Fisica, Università di Torino, Via P. Giuria 1, 10125 Torino, Italy 2 Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy e-mail: [email protected],[email protected] Received 31 January 2020 / Accepted 25 May 2020 ABSTRACT We derive the distribution of the phantom dark matter in the eight classical dwarf galaxies surrounding the Milky Way, under the assumption that modified Newtonian dynamics (MOND) is the correct theory of gravity. According to their observed shape, we model the dwarfs as axisymmetric systems, rather than spherical systems, as usually assumed. In addition, as required by the assumption of the MOND framework, we realistically include the external gravitational field of the Milky Way and of the large-scale structure beyond the Local Group. For the dwarfs where the external field dominates over the internal gravitational field, the phantom dark matter has, from the star distribution, an offset of ∼0:1−0:2 kpc, depending on the mass-to-light ratio adopted. This offset is a substantial fraction of the dwarf half-mass radius. For Sculptor and Fornax, where the internal and external gravitational fields are comparable, the phantom dark matter distribution appears disturbed with spikes at the locations where the two fields cancel each other; these features have little connection with the distribution of the stars within the dwarfs.
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Searching for Diffuse Light in the M96 Group
Draft version June 30, 2016 Preprint typeset using LATEX style emulateapj v. 5/2/11 SEARCHING FOR DIFFUSE LIGHT IN THE M96 GALAXY GROUP Aaron E. Watkins1, J. Christopher Mihos1,Paul Harding1,John J. Feldmeier2 Draft version June 30, 2016 ABSTRACT We present deep, wide-field imaging of the M96 galaxy group (also known as the Leo I Group). Down to surface brightness limits of µB = 30:1 and µV = 29:5, we find no diffuse, large-scale optical counterpart to the “Leo Ring”, an extended HI ring surrounding the central elliptical M105 (NGC 3379). However, we do find a number of extremely low surface-brightness (µB & 29) small-scale streamlike features, possibly tidal in origin, two of which may be associated with the Ring. In addition we present detailed surface photometry of each of the group’s most massive members – M105, NGC 3384, M96 (NGC 3368), and M95 (NGC 3351) – out to large radius and low surface brightness, where we search for signatures of interaction and accretion events. We find that the outer isophotes of both M105 and M95 appear almost completely undisturbed, in contrast to NGC 3384 which shows a system of diffuse shells indicative of a recent minor merger. We also find photometric evidence that M96 is accreting gas from the HI ring, in agreement with HI data. In general, however, interaction signatures in the M96 Group are extremely subtle for a group environment, and provide some tension with interaction scenarios for the formation of the Leo HI Ring. The lack of a significant component of diffuse intragroup starlight in the M96 Group is consistent with its status as a loose galaxy group in which encounters are relatively mild and infrequent.
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Is There Tension Between Observed Small Scale Structure and Cold Dark Matter?
Is there tension between observed small scale structure and cold dark matter? Louis Strigari Stanford University Cosmic Frontier 2013 March 8, 2013 Predictions of the standard Cold Dark Matter model 26 3 1 1. Density profiles rise towards the centersσannv 3of 10galaxies− cm s− (1) h i' ⇥ ⇢ Universal for all halo masses ⇢(r)= s (2) (r/r )(1 + r/r )2 Navarro-Frenk-White (NFW) model s s 2. Abundance of ‘sub-structure’ (sub-halos) in galaxies Sub-halos comprise few percent of total halo mass Most of mass contained in highest- mass sub-halos Subhalo Mass Function Mass[Solar mass] 1 Problems with the standard Cold Dark Matter model 1. Density of dark matter halos: Faint, dark matter-dominated galaxies appear less dense that predicted in simulations General arguments: Kleyna et al. MNRAS 2003, 2004;Goerdt et al. APJ2006; de Blok et al. AJ 2008 Dwarf spheroidals: Gilmore et al. APJ 2007; Walker & Penarrubia et al. APJ 2011; Angello & Evans APJ 2012 2. ‘Missing satellites problem’: Simulations have more dark matter subhalos than there are observed dwarf satellite galaxies Earilest papers: Kauffmann et al. 1993; Klypin et al. 1999; Moore et al. 1999 Solutions to the issues in Cold Dark Matter 1. The theory is wrong i) Not enough physics in theory/simulations (Talks yesterday by M. Boylan-Kolchin, M. Kuhlen) [Wadepuhl & Springel MNRAS 2011; Parry et al. MRNAS 2011; Pontzen & Governato MRNAS 2012; Brooks et al. ApJ 2012] ii) Cosmology/dark matter is wrong (Talk yesterday by A. Peter) 2. The data is wrong i) Kinematics of dwarf spheroidals (dSphs) are more difficult than assumed ii) Counting satellites a) Many more faint satellites around the Milky Way b) Milky Way is an oddball [Liu et al.
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The Hubble Space Telescope Proper Motion Collaboration HSTPROMO
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Calendar of Roman Events
Introduction Steve Worboys and I began this calendar in 1980 or 1981 when we discovered that the exact dates of many events survive from Roman antiquity, the most famous being the ides of March murder of Caesar. Flipping through a few books on Roman history revealed a handful of dates, and we believed that to fill every day of the year would certainly be impossible. From 1981 until 1989 I kept the calendar, adding dates as I ran across them. In 1989 I typed the list into the computer and we began again to plunder books and journals for dates, this time recording sources. Since then I have worked and reworked the Calendar, revising old entries and adding many, many more. The Roman Calendar The calendar was reformed twice, once by Caesar in 46 BC and later by Augustus in 8 BC. Each of these reforms is described in A. K. Michels’ book The Calendar of the Roman Republic. In an ordinary pre-Julian year, the number of days in each month was as follows: 29 January 31 May 29 September 28 February 29 June 31 October 31 March 31 Quintilis (July) 29 November 29 April 29 Sextilis (August) 29 December. The Romans did not number the days of the months consecutively. They reckoned backwards from three fixed points: The kalends, the nones, and the ides. The kalends is the first day of the month. For months with 31 days the nones fall on the 7th and the ides the 15th. For other months the nones fall on the 5th and the ides on the 13th.
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The Beginners Guide to Astrology AQUARIUS JAN
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Hubble Space Telescope Observations of the Local Group
THE ASTROPHYSICAL JOURNAL, 514:665È674, 1999 April 1 ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. HUBBL E SPACE T EL ESCOPE OBSERVATIONS OF THE LOCAL GROUP DWARF GALAXY LEO I CARME GALLART,1 WENDY L. FREEDMAN,1 MARIO MATEO,2 CESARE CHIOSI,3 IAN B. THOMPSON,1 ANTONIO APARICIO,4 GIANPAOLO BERTELLI,3,5 PAUL W. HODGE,6 MYUNG G. LEE,7 EDWARD W. OLSZEWSKI,8 ABHIJIT SAHA,9 PETER B. STETSON,10 AND NICHOLAS B. SUNTZEFF11 Received 1998 March 19; accepted 1998 November 6 ABSTRACT We present deep HST F555W (V ) and F814W (I) observations of a central Ðeld in the Local Group dwarf spheroidal (dSph) galaxy Leo I. The resulting color-magnitude diagram (CMD) reaches I ^ 26 and reveals the oldest ^10È15 Gyr old turno†s. Nevertheless, a horizontal branch is not obvious in the CMD. Given the low metallicity of the galaxy, this likely indicates that the Ðrst substantial star forma- tion in the galaxy may have been somehow delayed in Leo I in comparison with the other dSph satel- lites of the Milky Way. The subgiant region is well and uniformly populated from the oldest turno†s up to the 1 Gyr old turno†, indicating that star formation has proceeded in a continuous way, with possible variations in intensity but no big gaps between successive bursts, over the galaxyÏs lifetime. The structure of the red clump of core He-burning stars is consistent with the large amount of intermediate-age popu- lation inferred from the main sequence and the subgiant region.
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Streaming Motion in Leo I
The Annals of Applied Statistics 2009, Vol. 3, No. 1, 96–116 DOI: 10.1214/08-AOAS211 © Institute of Mathematical Statistics, 2009 STREAMING MOTION IN LEO I BY BODHISATTVA SEN,1 MOULINATH BANERJEE,2 MICHAEL WOODROOFE,3 MARIO MATEO AND MATTHEW WALKER University of Michigan, University of Michigan, University of Michigan, University of Michigan, and University of Cambridge Whether a dwarf spheroidal galaxy is in equilibrium or being tidally dis- rupted by the Milky Way is an important question for the study of its dark matter content and distribution. This question is investigated using 328 re- cent observations from the dwarf spheroidal Leo I. For Leo I, tidal disruption is detected, at least for stars sufﬁciently far from the center, but the effect appears to be quite modest. Statistical tools include isotonic and split point estimators, asymptotic theory, and resampling methods. 1. Introduction. The dwarf spheroidal galaxies near the Milky Way are among the least luminous galaxies in the night sky. While they have stellar popu- lations similar to those of globular clusters, approximately 106–107 stars, they are considerably larger systems, typically hundreds, even thousands of parsecs in size compared to radii of tens of parsecs characteristic of clusters. They are excellent candidates for the study of dark matter because they are nearby and generally have extremely low stellar densities. Moreover, due to their proximity to the Milky Way, many of these dwarf galaxies are also potentially strongly affected by disruptive tidal effects. The mere existence of dwarf spheroidal galaxies suggests these sys- tems contain much dark matter since it is unclear how they could have avoided the effects of tidal disruption without the added gravitational force from a consider- able reservoir of unseen matter [see Muñoz, Majewski and Johnston (2008)and Mateo, Olszewski and Walker (2008)].
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Neutral Hydrogen in Local Group Dwarf Galaxies
Neutral Hydrogen in Local Group Dwarf Galaxies Jana Grcevich Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2013 c 2013 Jana Grcevich All rights reserved ABSTRACT Neutral Hydrogen in Local Group Dwarfs Jana Grcevich The gas content of the faintest and lowest mass dwarf galaxies provide means to study the evolution of these unique objects. The evolutionary histories of low mass dwarf galaxies are interesting in their own right, but may also provide insight into fundamental cosmological problems. These include the nature of dark matter, the disagreement be- tween the number of observed Local Group dwarf galaxies and that predicted by ΛCDM, and the discrepancy between the observed census of baryonic matter in the Milky Way’s environment and theoretical predictions. This thesis explores these questions by studying the neutral hydrogen (HI) component of dwarf galaxies. First, limits on the HI mass of the ultra-faint dwarfs are presented, and the HI content of all Local Group dwarf galaxies is examined from an environmental standpoint. We find that those Local Group dwarfs within 270 kpc of a massive host galaxy are deficient in HI as compared to those at larger galactocentric distances. Ram- 4 3 pressure arguments are invoked, which suggest halo densities greater than 2-3 10− cm− × out to distances of at least 70 kpc, values which are consistent with theoretical models and suggest the halo may harbor a large fraction of the host galaxy’s baryons. We also find that accounting for the incompleteness of the dwarf galaxy count, known dwarf galaxies whose gas has been removed could have provided at most 2.1 108 M of HI gas to the Milky Way.
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Searches for HI in the Outer Parts of Four Dwarf Spheroidal Galaxies
Searches for HI in the Outer Parts of Four Dwarf Spheroidal Galaxies L. M. Young Astronomy Department (MSC 4500), New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003; [email protected] ABSTRACT Previous searches for atomic gas in our Galaxy’s dwarf spheroidal companions have not been complete enough to settle the question of whether or not these galaxies have HI, especially in their outer parts. We present new observations of the dwarf spheroidals Sextans, Leo I, Ursa Minor, and Draco, using the NRAO 140-foot telescope to search much farther in radius than has been done before. The new data go out to at least 2.5 times the core radius in all cases, and well beyond even the tidal radius in two cases. These observations give HI column density limits of 2–6×1017 cm−2. Unless HI is quite far from the galaxies’ centers, we conclude that these galaxies don’t contain signiﬁcant amounts of atomic gas at the present time. We discuss whether the observations could have missed some atomic gas. 1. Introduction Our Galaxy’s dwarf spheroidal companions have long been thought to be old and dead galaxies. They show no evidence for current star formation. Furthermore, searches for HI arXiv:astro-ph/9910398v1 21 Oct 1999 emission from the dwarf spheroidal galaxies found no evidence of neutral gas (Knapp et al. 1978; Mould et al. 1990; Koribalski, Johnston, & Otrupcek 1994); one exception seems to be Sculptor (Carignan et al. 1998). Optical and UV absorption experiments for Leo I (Bowen et al.
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Galaxy Group and Cluster Astronomy at RIT
Galaxy Group and Cluster Astronomy at RIT 23 Spitzer,)HST,)GALEX,)&)Chandra)Image) Green Bank 100M Hershel 3.5M Credit:)NRAO) Credit:)Chicago)University) Hubble Space Telescope (HST) Sloan Digital 2.4M Sky Survey 2.5M Credit:) Hubblesite ) In Space On Earth Astronomers at RIT want to learn about galaxy groups and clusters. They use a variety of ground- and space-based telescopes. 24 YOU ARE HERE Milky Way galaxy Artist’s representation Here’s where the sun lives! We are on the outskirts of the Milky Way. It takes the sun 200 million years to travel once around the galaxy. Credit:)NASA/JPLJCaltech/R) 25 Sometimes galaxies run past each other or even combine! ZOOM Antennae Galaxies This can jumpstart star formation and make irregularly shaped galaxies like the ones shown here. 26 Credit:)HubbleSite) Living as a group of galaxies, the Milky Way has neighbors: the larger Andromeda and the smaller Tr i a n g u l u m . The Milky Way s Home The Local Group Andromeda Galaxy This is an artist’s interpretation. NGC185 Not drawn to scale. NGC147 M32 Tr i a n g u l u m Galaxy NGC205 Pegasus Milky Way Galaxy IC1613 Draco Fornax WLM Ursa Minor Sculptor LEo I Leo II Sextans NGC6822 SMC LMC Carina Artist’s representation of the Local Group Around each larger galaxy there are dozens of dwarf galaxies. It takes light 2.5 million years to get to Earth from Andromeda. 27 Hundreds, or even thousands, of galaxies can live together in a cluster. A crowded neighborhood Abell 1689 shown here has over 2000 galaxies living far, far away from Earth.
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Dissecting the Stellar Content of Leo I: a Dwarf Irregular Caught in Transition
MNRAS 000,1{19 (2020) Preprint 16 December 2020 Compiled using MNRAS LATEX style file v3.0 Dissecting the stellar content of Leo I: a dwarf irregular caught in transition T. Ruiz-Lara1;2;3?, C. Gallart2;3, M. Monelli2;3, T. K. Fritz2;3, G. Battaglia2;3, S. Cassisi4;5, M. Luis Aznar2, A. V. Russo Cabrera2;6, I. Rodr´ıguez-Mart´ın7, J. J. Salazar-González7 1 Kapteyn Astronomical Institute, University of Groningen, Landleven 12, 9747 AD Groningen, The Netherlands 2 Instituto de Astrof´ısica de Canarias, Calle V´ıaLáctea s/n, E-38205 La Laguna, Tenerife, Spain 3 Departamento de Astrof´ısica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain 4 INAF { Astronomical Observatory of Abruzzo, via M. Maggini, sn, 64100 Teramo, Italy 5 INFN, Sezione di Pisa, Largo Pontecorvo 3, 56127 Pisa, Italy 6 Grupo de Operaciones de Ingenier´ıa, Gran Telescopio de Canarias, Cuesta de San José, s/n, E-38712 Bre~naBaja, La Palma, Spain 7 Dpto. de Matemáticas, Estad´ıstica e Investigación Operativa, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain Accepted 2020 November 24. Received 2020 November 24; in original form 2020 October 13 ABSTRACT Leo I is considered one of the youngest dwarf spheroidals (dSph) in the Local Group. Its isolation, extended star formation history (SFH), and recent perigalacticon passage (∼1 Gyr ago) make Leo I one of the most interesting nearby stellar systems. Here, we analyse deep photometric Hubble Space Telescope data via colour-magnitude diagram fitting techniques to study its global and radially-resolved SFH.
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