Editorial Satish Pande Kiran Ghadge ©

Total Page:16

File Type:pdf, Size:1020Kb

Editorial Satish Pande Kiran Ghadge © ISSN 2319-4361 (Indexed in Google Scholar) Volume 3 | Issue 3 | August - October 2014 Editorial Satish Pande Kiran Ghadge © Male White-bellied Minivet he low populations of Gyps vultures remain a cause forest departments with the participation of the local Tof concern. There is some evidence that the declining people and NGO’s. Many breeding sites of cliff nesting trend has now stabilized. To effectively promote vulture and tree nesting Gyps species are in private ownership conservation all present vulture breeding sites need to plots. The involvement of local communities is the be identifi ed urgently. These sites can then be prioritized pivot of vulture conservation. for protection and future conservation. Problems that Continued monitoring of such sites is possible such breeding sites may be facing can be identifi ed and with the active enthusiastic participation of sensitized appropriate measures can be taken by the respective local youth. Monitoring includes gathering data on Ela Journal / www.elafoundation.org / Vol. 3 Issue 3 / August - October 2014 | 1 EDITORIAL commencement of breeding, number of breeding pairs, activities are threatening natural habitats on an occupation of nests, incubation and hatching, food unprecedented scale. Small habitat pockets are the last availability, threats to nestlings, protection of nest trees resorts of several species. There are several other avian and provisioning of carcasses for feeding in case of species about which ornithological data on aspects food shortage. such as habitat preference, feeding and breeding Provisioning of food at vulture restaurants in the form ecology, population recruitment success and threats of dead and diclofenac-free carcasses can be done at the is not available. Studies to gather such vital data are local level. The government machinery, particularly the important for effective conservation of species. forest department, is quite understaffed and they depend The key to safeguarding species for future lies in on local feedbacks for the availability of fresh carcass. getting scientifi c data and imparting education to our The problem of handling and the cost of transport of rural folk by ‘Rural Outreach Biodiversity Conservation carcasses can be jointly solved by local people and Workshops’. Ela Foundation has already completed forest offi cials, provided the economic burden is borne rural outreach programs in the towns of Jejuri, Baramati, by the forest department. The handling of putrefying Yadavwadi, with more than 100 participants each, and carcasses is a demanding task, and I have personal at Varanasi in Uttar Pradesh, with 250 participants, experience of the suffocating odor and the diffi culty in from surrounding 20 or more villages in each region. lifting dead animals. Availability of vehicles is not easy Several future rural outreach workshops are in the and people are often reluctant to offer vehicles to carry pipeline. These interactive programs have become out the unhygienic job of transport of cattle or other popular. They create sensitization and awareness animal carcass. about the conservation of habitats, need for conserving Other important manpower-free studies are biodiversity, importance of species, methods of study, continued observations by deploying motion sensing and use of ethno-biological perspective for conservation cameras on a few randomly selected nests of various among the rural communities. \ vulture species. This will throw light on the behavior Keeping with the above philosophy, in this issue, of breeding vultures at nests. So also, presently, we do we have papers on the discovery of nests of the Red- not have any data on the movement of vultures in India, headed Vulture in Nepal and the implementation particularly the home range and feeding areas of adults of conservation awareness programs in rural areas; and the dispersal range of young. This is possible only we have new ornithological data on the less known by satellite transmitters fi tted on vultures. The forest White-bellied Minivet from rural India, among others. department should promote such studies on a priority The papers exemplify that the out come of efforts of and the ornithological expertise can be taken from the village-based people interested in nature studies and experts from outside the department, if such critical conservation provide valuable scientifi c inputs – truly knowledge is not available in the department. Peoples’ Science for Nature Conservation. Today, widespread and increasing anthropological 2 | Ela Journal / www.elafoundation.org / Vol. 3 Issue 3 / August - October 2014 ETHNO-ORNITHOLOGY Ganga and Makara Dr. Suruchi Pande* *Ethno-Ornithilogist and Sanskrit scholar Citation: Pande, Suruchi (2014). In Indian culture Makara (a crocodile) is believed Ganga and Makara Ela Journal 3(3):3-5. to be the vehicle of the holy river Ganga or the Ganges. The meaning of the Sanskrit word Ganga is “the one Date of Publication: who takes (us or the devotees) towards God”. In 01-10-2014 Indian culture, Makara is believed to be the symbol of lust and attachment. When we have controlled the lust ISSN 2319-4361 for worldly passions, we are set free and can persue higher goals in life. That is why Makara is said to be a Copyright: © Pande, Suruchi. carrier vehicle of Ganga, who has a control on it. Email: [email protected] Meaning of the word Makara Suruchi Pande © The painting of goddess Ganga with Makar in Vishrambagwada (Pune) Ela Journal / www.elafoundation.org / Vol. 3 Issue 3 / August - October 2014 | 3 Ganga and Makara ETHNO-ORNITHOLOGY Both Photos: Suruchi Pande © Goddess Ganga with Makar in a temple at Goddess Ganga with Ghadiyal in a temple on a Varanasi ghat, Varanasi 1 Makara Makaraketana- having the Makara for an emblem; a) An aquatic monster understood variably as the or having a fi sh on his banner. (MW, 1976, p. 771). alligator, crocodile or shark but properly, a fabulous animal. It is the emblem of the god of love- SYNONYMS Kamadeva. The lexicon Amarakosha (1/10/20 and 1/10/21) says, b) One of the signs of the zodiac. It corresponds with Shishumara = a child-killer, the Gangetic porpoise Capricorn. (Molesworth, 1975, p.624). or a dolphin or an alligator. (MW) Udra = an aquatic animal or a crab or an otter. 2 Nakra- Magar or Susar. A crocodile. [in other (MW). languages : Sanskrit- Nakra; Kannada- Negar; Tulu- Shanku = an aquatic animal. Negalu]. ) (Kulkarni, K. P., Vol.II, year- ? p.469). ‘Nakrastu kumbhirah|’ = ‘kumbhira’ is a crocodile of the Ganges (the long-nosed alligator). 3 Nakra – a crocodile, an alligator. Nakraketana- All these are called as ‘jala jantu’ – aquatic Name of god of love. (MW, 1976, p. 524) animals. Makara- a kind of sea monster (sometimes confounded with the crocodile, shark or dolphin; ETYMOLOGY regarded as the emblem of Kamadeva). If we see the root verb in Makara it is ‘makam rati’| 4 | Ela Journal / www.elafoundation.org / Vol. 3 Issue 3 / August - October 2014 Ganga and Makara ORNITHOLOGY = Ra or Ras cl. 2 P = to grant, to give, to bestow or to and Neela kamala. impart. (BSK, vol.II, p. 257). The verb in ‘kumbhira’ is ‘irati’ means to go, to move, to arise from. A variation of ‘kumbhira’ is I have not yet come across any other mythological ‘kumbhila’. The verb in this word ‘ilati’ means ‘not story except in the Ananda Ramayana explaining to move’. the signifi cance of depicting a Makara on the fl ag of The text Abhidhanacintamani (4.417) says, Kamadeva. But there is a possibility to fi nd one in the ‘Mankate makarah|’ = The root verb ‘mank’ means to vast literature depicting Hindu mythology. move or to adorn. English word Muggar is for the fresh water REFERENCES crocodile. A Sanskrit-English Dictionary, M. Monier- In Hindi the word Magar is used. Williams 1899(1976), Delhi: Motilal Banarsidass. From ‘makar to magar’. I think here we go from (Abbreviation MW). a harsh letter of alphabet to the soft letter.- (from ‘ka’ to ‘ga’ according to letters in the Marathi language. Abhidhanachintamani. Vol.I, II Of (This may not have grammatical justifi cation.). Hemachandracharya, ed. Hargovindas et al.(Veer I have found that in Farsi language ‘maga’ means Era 2441, 2446), Bhavanagar: Vakil, N. L. and a small river. Sheth P. R. & Sheth C. P. The Ashtadhyayi of Panini mentions nakra as ‘na kramati’| (VI.3.75). (Panini/Vasu,1988, vol. II, p. Amarakosha. Pandita varasrimadamarasimhaviracitah 1233). ‘Na kramati’ means not moving, in allusion to Namalinganusasanam Nama Amarakosa, ed. the habit of the crocodile of staying still at one place Haragovind Sastri (1957), Varanasi: Chowkhamba without moving. Sanskrit Series Offi ce. MYTHOLOGY Ananda Ramayanam. Hindi trans. Ramtej Sastri a) ‘Makaradhvaja’ is son of Hanumana. He was Pandeya (1966), Kashi: Pandit Pustakalaya. born to a crocodile that was residing in the ocean Bharatiya Sanskruti Kosha. Vol.II, ed. Pt. (salt-water crocodile) as the drops of perspiration Mahadevasastri Joshi (1985), Pune: Bharatiya of Hanuman fell on her body. (Vettam Mani,1989, Sanskruti Kosha Mandal. (Abbreviation BSK). p.471). The original story is found in the Ananda Ramayana Marathi Etymological Dictionary. Vol. II, Kulkarni, (SaraKanda, Canto 11, verses83-90). K. P. (year?), Mumbai: Keshav bhikaji Dhavale. b) The same text has another story where a sage Molesworth’s Marathi-English Dictionary, corrected makes an immoral demand to a beautiful Apsara print 1831 (1975), Pune: Shubhada-Saraswat Publ. (heavenly damsel) named ‘Dhanyamali’. But she declines to accept and the angry sage curses her to Puranic Encyclopaedia. Vettam mani (1989), Delhi: become a crocodile. God Hanumana frees her spirit Motilal Banarsidass. by killing the crocodile in whose body the Apsara is trapped. She regains her heavenly form. (Ananda The Astadhyayi Of Panini. Vol. II, ed and Engl, Ramayana, SaraKanda, Canto 11, verses 54-56). trans. Srisa Chandra Vasu 1891(1988), Delhi: Motilal Banarsidass. ICONOGRAPHY With the fl ag bearing idol of the Kamadeva., a Makara is depicted on his fl ag and the face of the Makar is made up of fi ve arrows.
Recommended publications
  • Mathématiques Et Espace
    Atelier disciplinaire AD 5 Mathématiques et Espace Anne-Cécile DHERS, Education Nationale (mathématiques) Peggy THILLET, Education Nationale (mathématiques) Yann BARSAMIAN, Education Nationale (mathématiques) Olivier BONNETON, Sciences - U (mathématiques) Cahier d'activités Activité 1 : L'HORIZON TERRESTRE ET SPATIAL Activité 2 : DENOMBREMENT D'ETOILES DANS LE CIEL ET L'UNIVERS Activité 3 : D'HIPPARCOS A BENFORD Activité 4 : OBSERVATION STATISTIQUE DES CRATERES LUNAIRES Activité 5 : DIAMETRE DES CRATERES D'IMPACT Activité 6 : LOI DE TITIUS-BODE Activité 7 : MODELISER UNE CONSTELLATION EN 3D Crédits photo : NASA / CNES L'HORIZON TERRESTRE ET SPATIAL (3 ème / 2 nde ) __________________________________________________ OBJECTIF : Détermination de la ligne d'horizon à une altitude donnée. COMPETENCES : ● Utilisation du théorème de Pythagore ● Utilisation de Google Earth pour évaluer des distances à vol d'oiseau ● Recherche personnelle de données REALISATION : Il s'agit ici de mettre en application le théorème de Pythagore mais avec une vision terrestre dans un premier temps suite à un questionnement de l'élève puis dans un second temps de réutiliser la même démarche dans le cadre spatial de la visibilité d'un satellite. Fiche élève ____________________________________________________________________________ 1. Victor Hugo a écrit dans Les Châtiments : "Les horizons aux horizons succèdent […] : on avance toujours, on n’arrive jamais ". Face à la mer, vous voyez l'horizon à perte de vue. Mais "est-ce loin, l'horizon ?". D'après toi, jusqu'à quelle distance peux-tu voir si le temps est clair ? Réponse 1 : " Sans instrument, je peux voir jusqu'à .................. km " Réponse 2 : " Avec une paire de jumelles, je peux voir jusqu'à ............... km " 2. Nous allons maintenant calculer à l'aide du théorème de Pythagore la ligne d'horizon pour une hauteur H donnée.
    [Show full text]
  • 100 Closest Stars Designation R.A
    100 closest stars Designation R.A. Dec. Mag. Common Name 1 Gliese+Jahreis 551 14h30m –62°40’ 11.09 Proxima Centauri Gliese+Jahreis 559 14h40m –60°50’ 0.01, 1.34 Alpha Centauri A,B 2 Gliese+Jahreis 699 17h58m 4°42’ 9.53 Barnard’s Star 3 Gliese+Jahreis 406 10h56m 7°01’ 13.44 Wolf 359 4 Gliese+Jahreis 411 11h03m 35°58’ 7.47 Lalande 21185 5 Gliese+Jahreis 244 6h45m –16°49’ -1.43, 8.44 Sirius A,B 6 Gliese+Jahreis 65 1h39m –17°57’ 12.54, 12.99 BL Ceti, UV Ceti 7 Gliese+Jahreis 729 18h50m –23°50’ 10.43 Ross 154 8 Gliese+Jahreis 905 23h45m 44°11’ 12.29 Ross 248 9 Gliese+Jahreis 144 3h33m –9°28’ 3.73 Epsilon Eridani 10 Gliese+Jahreis 887 23h06m –35°51’ 7.34 Lacaille 9352 11 Gliese+Jahreis 447 11h48m 0°48’ 11.13 Ross 128 12 Gliese+Jahreis 866 22h39m –15°18’ 13.33, 13.27, 14.03 EZ Aquarii A,B,C 13 Gliese+Jahreis 280 7h39m 5°14’ 10.7 Procyon A,B 14 Gliese+Jahreis 820 21h07m 38°45’ 5.21, 6.03 61 Cygni A,B 15 Gliese+Jahreis 725 18h43m 59°38’ 8.90, 9.69 16 Gliese+Jahreis 15 0h18m 44°01’ 8.08, 11.06 GX Andromedae, GQ Andromedae 17 Gliese+Jahreis 845 22h03m –56°47’ 4.69 Epsilon Indi A,B,C 18 Gliese+Jahreis 1111 8h30m 26°47’ 14.78 DX Cancri 19 Gliese+Jahreis 71 1h44m –15°56’ 3.49 Tau Ceti 20 Gliese+Jahreis 1061 3h36m –44°31’ 13.09 21 Gliese+Jahreis 54.1 1h13m –17°00’ 12.02 YZ Ceti 22 Gliese+Jahreis 273 7h27m 5°14’ 9.86 Luyten’s Star 23 SO 0253+1652 2h53m 16°53’ 15.14 24 SCR 1845-6357 18h45m –63°58’ 17.40J 25 Gliese+Jahreis 191 5h12m –45°01’ 8.84 Kapteyn’s Star 26 Gliese+Jahreis 825 21h17m –38°52’ 6.67 AX Microscopii 27 Gliese+Jahreis 860 22h28m 57°42’ 9.79,
    [Show full text]
  • Debris Dust Around Main Sequence Stars
    Debris Dust Around Main Sequence Stars et al. (2013) Kalas Chris5ne H. Chen STScI, September 2016 1 Exoplanetary Systems Exoplanet Observaons Debris Disk Observaons 2 Outline • The HR 4796 System • Training Students Using the KecK LWS • Spitzer GTO Programs – A Search for Terrestrial Planetary Debris Systems and Other Planetary Debris DisKs – Spectroscopy of Protostellar, Protoplanetary and Debris DisKs – Dust Around Main Sequence A-type Stars – The Fabulous Four Debris DisKs 3 Early Debris DisK WorK Timeline • 1983 IRAS launches • 1984 Smith & Terrile spaally resolve the β Pic disK in scaered light using a coronagraph • 1986 Gille] accurately measures “infrared excess” toward Vega, Fomalhaut and β Pic from pointed IRAS observaons • 1991 Jura discovers HR 4796 IRAS infrared excess • 1991 Telesco and KnacKe discover spectroscopic evidence for silicates around β Pic • 1993 BacKman review ar5cle “Main Sequence Stars with Circumstellar Solid Material: The Vega Phenomenon” is published in Protostars and Planets III • 1998 Koerner and Jayawardhana resolve the HR 4796A disK in thermal emission using KecK/MIRLIN and Blanco/OSCIR • 2003 Spitzer launches • 2014 Gemini Planet Imager commissioning HR 4796A Infrared Excess Discovery HR 4796B Secondary Star Discovery • First es5mate for the grain temperature based on simple blacK body modeling, Tgr = 110 K with a predic5on for the distance of the grains from the star, ~40 AU • First grain size constrain (> 10 μm) based on the upper limit for the size of the system (<5” at 20 μm) • First calculaon of the Poyn5ng-Robertson drag life5me for this disK demonstrang that it must be a debris disK HR 4796A Planetary Companion Constraints • Central clearing may be created by a planetary mass object • SpecKle observaons constrain the mass to be < 0.125 M¤ The HR 4796A DisK Resolved! (Leo) HST NICMOS F1600W and F1100W coronagraphic images showing discovery of the light scaered from the dust (Schneider et al.
    [Show full text]
  • NGC 6872 in the Constellation of Pavo 23 September 2014
    Image: NGC 6872 in the constellation of Pavo 23 September 2014 of free hydrogen, which is the basis material for new stars, meaning that if it weren't for its interactions with IC 4970, NGC 6872 might not have been able to produce new bursts of star formation. Provided by NASA Credit: ESA/Hubble & NASA / Acknowledgement: Judy Schmidt This picture, taken by the NASA/ESA Hubble Space Telescope's Wide Field Planetary Camera 2 (WFPC2), shows a galaxy known as NGC 6872 in the constellation of Pavo (The Peacock). Its unusual shape is caused by its interactions with the smaller galaxy that can be seen just above NGC 6872, called IC 4970. They both lie roughly 300 million light-years away from Earth. From tip to tip, NGC 6872 measures over 500,000 light-years across, making it the second largest spiral galaxy discovered to date. In terms of size it is beaten only by NGC 262, a galaxy that measures a mind-boggling 1.3 million light-years in diameter! To put that into perspective, our own galaxy, the Milky Way, measures between 100,000 and 120,000 light-years across, making NGC 6872 about five times its size. The upper left spiral arm of NGC 6872 is visibly distorted and is populated by star-forming regions, which appear blue on this image. This may have been be caused by IC 4970 recently passing through this arm—although here, recent means 130 million years ago! Astronomers have noted that NGC 6872 seems to be relatively sparse in terms 1 / 2 APA citation: Image: NGC 6872 in the constellation of Pavo (2014, September 23) retrieved 23 September 2021 from https://phys.org/news/2014-09-image-ngc-constellation-pavo.html This document is subject to copyright.
    [Show full text]
  • The Solitary G-Mode Frequencies in Early B-Type Stars
    The solitary g-mode frequencies in early B-type stars J. Daszy´nska-Daszkiewicz1, P. Walczak1, A. Pamyatnykh2, M. Jerzykiewicz1, A. Pigulski1 and the BRITE Team 1. Instytut Astronomiczny, Uniwersytet Wroc lawski, Kopernika 11, 51-622 Wroc law, Poland 2. Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00{716 Warszawa, Poland We present possible explanations of pulsations in early B-type main sequence stars which arise purely from the excitation of gravity modes. There are three stars with this type of oscillations detected from the BRITE light curves: κ Cen, a Car, and κ Vel. We show that by changing metallicity or the opacity profile it is possible in some models to dump pressure modes keeping gravity modes unstable. Other possible scenario involves pulsations of a lower mass companion. 1 Introduction For many years, it seemed that B-type main sequence (MS) pulsators can be divided into two groups: β Cephei stars with low-order pressure (p) and/or gravity (g) mode pulsations (e.g., Moskalik & Dziembowski, 1992; Stankov & Handler, 2005) and Slowly Pulsating B-type stars (SPB) with high-order g-mode pulsations (Waelkens, 1991; Dziembowski et al., 1993). This simple dichotomy was spoiled by the continuous increase in accuracy of the time-series photometry obtained from multi-site campaigns and, mainly, from space missions (CoRoT, Kepler, BRITE). Thereby, many pulsators with so far unknown oscillation spectra were identified. The first example are hybrid pulsators with low order p=g-modes and high-order g-modes excited simultaneously. Then, even more unexpected by theoretical models oscillation spectra were obtained from the CoRoT and Kepler space data: late B-type stars with only high frequencies and early B-type stars with only low frequencies (Degroote et al., 2009; Balona et al., 2011, 2015).
    [Show full text]
  • The Brightest Stars Seite 1 Von 9
    The Brightest Stars Seite 1 von 9 The Brightest Stars This is a list of the 300 brightest stars made using data from the Hipparcos catalogue. The stellar distances are only fairly accurate for stars well within 1000 light years. 1 2 3 4 5 6 7 8 9 10 11 12 13 No. Star Names Equatorial Galactic Spectral Vis Abs Prllx Err Dist Coordinates Coordinates Type Mag Mag ly RA Dec l° b° 1. Alpha Canis Majoris Sirius 06 45 -16.7 227.2 -8.9 A1V -1.44 1.45 379.21 1.58 9 2. Alpha Carinae Canopus 06 24 -52.7 261.2 -25.3 F0Ib -0.62 -5.53 10.43 0.53 310 3. Alpha Centauri Rigil Kentaurus 14 40 -60.8 315.8 -0.7 G2V+K1V -0.27 4.08 742.12 1.40 4 4. Alpha Boötis Arcturus 14 16 +19.2 15.2 +69.0 K2III -0.05 -0.31 88.85 0.74 37 5. Alpha Lyrae Vega 18 37 +38.8 67.5 +19.2 A0V 0.03 0.58 128.93 0.55 25 6. Alpha Aurigae Capella 05 17 +46.0 162.6 +4.6 G5III+G0III 0.08 -0.48 77.29 0.89 42 7. Beta Orionis Rigel 05 15 -8.2 209.3 -25.1 B8Ia 0.18 -6.69 4.22 0.81 770 8. Alpha Canis Minoris Procyon 07 39 +5.2 213.7 +13.0 F5IV-V 0.40 2.68 285.93 0.88 11 9. Alpha Eridani Achernar 01 38 -57.2 290.7 -58.8 B3V 0.45 -2.77 22.68 0.57 144 10.
    [Show full text]
  • Studies on the Formation, Evolution, and Destruction of Massive Star Clusters Cover: Photograph Taken at White Sands, New Mexico
    Studies on the Formation, Evolution, and Destruction of Massive Star Clusters Cover: Photograph taken at White Sands, New Mexico. Courtesy of Matt Robertson. Printed by MultiCopy, Utrecht ISBN 90–393–0502–1 Studies on the Formation, Evolution, and Destruction of Massive Star Clusters Studie van de Vorming, Evolutie, en Destructie van Massieve Sterclusters (met een samenvatting in het Nederlands) Proefschrift ter verkrijging van de graad van doctor aan de Universiteit Utrecht op gezag van de Rector Magnificus, Prof. Dr. W.H. Gispen, ingevolge het besluit van het College voor Promoties in het openbaar te verdedigen op donderdag 21 april 2005 des middags te 12.45 uur door Nathan John Bastian geboren op 22 March 1978, te Milwaukee Promoter: prof. dr Henny J.G.L.M. Lamers Sterrenkundig Instituut, Universiteit Utrecht Co-Promoter: dr Markus Kissler-Patig European Southern Observatory This research has been supported in part by the Nether- lands Organization for Scientific Research (NWO). Additional support has come from the European South- ern Observatory (ESO). Contents 1 Introduction 1 1.1 Introduction to Extragalactic Star Clusters . 1 1.1.1 The Milky Way Bias . 1 1.1.2 The copious environments of young star clusters . 2 1.2 This Thesis . 5 1.2.1 Cluster Populations . 5 1.2.2 Dynamical Studies of the Massive Star Cluster W3 in the Merger Remnant NGC 7252 . 10 1.2.3 Cluster Complexes . 10 1.2.4 Future Plans . 13 Part A: The Cluster Population of M 51 15 2 Clusters in the Inner Spiral Arms of M 51: The cluster IMF and the formation history 17 2.1 Introduction .
    [Show full text]
  • Sirius Astronomer
    FEBRUARY 2013 Free to members, subscriptions $12 for 12 Volume 40, Number 2 Jupiter is featured often in this newsletter because it is one of the most appealing objects in the night sky even for very small telescopes. The king of Solar System planets is prominent in the night sky throughout the month, located near Aldebaran in the constellation Taurus. Pat Knoll took this image on January 18th from his observing site at Kearney Mesa, California, using a Meade LX200 Classic at f/40 with a 4X Powermate. The image was compiled from a two-minute run with an Imaging Source DFK 21AU618.AS camera . OCA CLUB MEETING STAR PARTIES COMING UP The free and open club meeting The Black Star Canyon site will open The next session of the Beginners will be held February 8 at 7:30 PM on February 2. The Anza site will be Class will be held at the Heritage in the Irvine Lecture Hall of the open on February 9. Members are en- Museum of Orange County at Hashinger Science Center at couraged to check the website calen- 3101 West Harvard Street in San- Chapman University in Orange. dar for the latest updates on star par- ta Ana on February 1st. The fol- This month, UCSD’s Dr. Burgasser ties and other events. lowing class will be held March will present “The Coldest Stars: Y- 1st Dwarfs and the Fuzzy Border be- Please check the website calendar for tween Stars and Planets.” the outreach events this month! Volun- GOTO SIG: TBA teers are always welcome! Astro-Imagers SIG: Feb.
    [Show full text]
  • Mid-IR Observations of Circumstellar Disks
    A&A 431, 175–182 (2005) Astronomy DOI: 10.1051/0004-6361:20041490 & c ESO 2005 Astrophysics Mid-IR observations of circumstellar disks II. Vega-type stars and a post-main sequence object O. Schütz1,G.Meeus2, and M. F. Sterzik3 1 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected] 2 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany 3 European Southern Observatory, Alonso de Cordova 3107, Santiago 19, Chile Received 18 June 2004 / Accepted 10 September 2004 Abstract. We present spectral energy distributions and new N-band photometry and spectroscopy for a sample of six main sequence stars and one post-MS object using the ESO TIMMI2 camera at La Silla observatory (Chile). All objects are thought to possess circumstellar material and for the majority of the targets this is their first N-band spectroscopic observation. The emission spectra (observed in three cases), modelled with a mixture of silicates consisting of different grain sizes and compo- sition, confirm the suspected presence of disks around these targets. The most important discovery is that HD 113766, a young Vega-type star, is host to highly processed dust which is probably second generation. It is the first time a Vega-type star with such highly evolved dust has been observed. Silicate emission of basically unevolved dust is seen in case of the post-MS object HD 41511 and the Vega-type star HD 172555. In addition, to study the cold dust, we observed a subsample at 1200 µm with the bolometer array SIMBA at the SEST in La Silla but we only got upper limits for those five objects.
    [Show full text]
  • The Co-Existence of Hot and Cold Gas in Debris Discs? I
    A&A 614, A3 (2018) https://doi.org/10.1051/0004-6361/201732329 Astronomy & © ESO 2018 Astrophysics The co-existence of hot and cold gas in debris discs? I. Rebollido1, C. Eiroa1, B. Montesinos2, J. Maldonado3, E. Villaver1, O. Absil4, A. Bayo5,6, H. Canovas1,7, A. Carmona8, Ch. Chen9, S. Ertel10, A. Garufi1, Th. Henning11, D. P. Iglesias5,6, R. Launhardt11, R. Liseau12, G. Meeus1, A. Moór13, A. Mora14, J. Olofsson5,6, G. Rauw4, and P. Riviere-Marichalar15 1 Departamento. Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, 28049 Madrid, Spain e-mail: [email protected] 2 Centro de Astrobiología (CAB, CSIC-INTA), ESAC Campus, Camino Bajo del Castillo s/n, Villanueva de la Cañada, 28692 Madrid, Spain 3 INAF, Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy 4 STAR Institute, Université de Liège, F.R.S.-FNRS, 19c Allée du Six Août, 4000 Liège, Belgium 5 Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Casilla, 5030 Valparaíso, Chile 6 Núcleo Milenio de Formación Planetaria-NPF, Universidad de Valparaíso, Av. Gran Bretaña, 1111 Valparaíso, Chile 7 European Space Astronomy Centre (ESA), PO Box 78, Villanueva de la Cañada, 28691 Madrid, Spain 8 Université de Toulouse, UPS-OMP, IRAP, 31400 Toulouse, France 9 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21212, USA 10 Steward Observatory, Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA 11 Max-Planck-Institut für Astronomie (MPIA), Königstuhl 17, 69117 Heidelberg, Germany 12 Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden 13 Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, PO Box 67, 1525 Budapest, Hungary 14 Aurora Technology B.V.
    [Show full text]
  • GTO Keypad Manual, V5.001
    ASTRO-PHYSICS GTO KEYPAD Version v5.xxx Please read the manual even if you are familiar with previous keypad versions Flash RAM Updates Keypad Java updates can be accomplished through the Internet. Check our web site www.astro-physics.com/software-updates/ November 11, 2020 ASTRO-PHYSICS KEYPAD MANUAL FOR MACH2GTO Version 5.xxx November 11, 2020 ABOUT THIS MANUAL 4 REQUIREMENTS 5 What Mount Control Box Do I Need? 5 Can I Upgrade My Present Keypad? 5 GTO KEYPAD 6 Layout and Buttons of the Keypad 6 Vacuum Fluorescent Display 6 N-S-E-W Directional Buttons 6 STOP Button 6 <PREV and NEXT> Buttons 7 Number Buttons 7 GOTO Button 7 ± Button 7 MENU / ESC Button 7 RECAL and NEXT> Buttons Pressed Simultaneously 7 ENT Button 7 Retractable Hanger 7 Keypad Protector 8 Keypad Care and Warranty 8 Warranty 8 Keypad Battery for 512K Memory Boards 8 Cleaning Red Keypad Display 8 Temperature Ratings 8 Environmental Recommendation 8 GETTING STARTED – DO THIS AT HOME, IF POSSIBLE 9 Set Up your Mount and Cable Connections 9 Gather Basic Information 9 Enter Your Location, Time and Date 9 Set Up Your Mount in the Field 10 Polar Alignment 10 Mach2GTO Daytime Alignment Routine 10 KEYPAD START UP SEQUENCE FOR NEW SETUPS OR SETUP IN NEW LOCATION 11 Assemble Your Mount 11 Startup Sequence 11 Location 11 Select Existing Location 11 Set Up New Location 11 Date and Time 12 Additional Information 12 KEYPAD START UP SEQUENCE FOR MOUNTS USED AT THE SAME LOCATION WITHOUT A COMPUTER 13 KEYPAD START UP SEQUENCE FOR COMPUTER CONTROLLED MOUNTS 14 1 OBJECTS MENU – HAVE SOME FUN!
    [Show full text]
  • Starshade Rendezvous Probe
    Starshade Rendezvous Probe Starshade Rendezvous Probe Study Report Imaging and Spectra of Exoplanets Orbiting our Nearest Sunlike Star Neighbors with a Starshade in the 2020s February 2019 TEAM MEMBERS Principal Investigators Sara Seager, Massachusetts Institute of Technology N. Jeremy Kasdin, Princeton University Co-Investigators Jeff Booth, NASA Jet Propulsion Laboratory Matt Greenhouse, NASA Goddard Space Flight Center Doug Lisman, NASA Jet Propulsion Laboratory Bruce Macintosh, Stanford University Stuart Shaklan, NASA Jet Propulsion Laboratory Melissa Vess, NASA Goddard Space Flight Center Steve Warwick, Northrop Grumman Corporation David Webb, NASA Jet Propulsion Laboratory Study Team Andrew Romero-Wolf, NASA Jet Propulsion Laboratory John Ziemer, NASA Jet Propulsion Laboratory Andrew Gray, NASA Jet Propulsion Laboratory Michael Hughes, NASA Jet Propulsion Laboratory Greg Agnes, NASA Jet Propulsion Laboratory Jon Arenberg, Northrop Grumman Corporation Samuel (Case) Bradford, NASA Jet Propulsion Laboratory Michael Fong, NASA Jet Propulsion Laboratory Jennifer Gregory, NASA Jet Propulsion Laboratory Steve Matousek, NASA Jet Propulsion Laboratory Jonathan Murphy, NASA Jet Propulsion Laboratory Jason Rhodes, NASA Jet Propulsion Laboratory Dan Scharf, NASA Jet Propulsion Laboratory Phil Willems, NASA Jet Propulsion Laboratory Science Team Simone D'Amico, Stanford University John Debes, Space Telescope Science Institute Shawn Domagal-Goldman, NASA Goddard Space Flight Center Sergi Hildebrandt, NASA Jet Propulsion Laboratory Renyu Hu, NASA
    [Show full text]