MEMORIA IAC 2013 Pero No Todo Son Balances Positivos
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The HARPS Search for Southern Extra-Solar Planets XXXV. The
Astronomy & Astrophysics manuscript no. santos_print c ESO 2021 July 9, 2021 The HARPS search for southern extra-solar planets.? XXXV. The interesting case of HD41248: stellar activity, no planets? N.C. Santos1; 2, A. Mortier1, J. P. Faria1; 2, X. Dumusque3; 4, V. Zh. Adibekyan1, E. Delgado-Mena1, P. Figueira1, L. Benamati1; 2, I. Boisse8, D. Cunha1; 2, J. Gomes da Silva1; 2, G. Lo Curto5, C. Lovis3, J. H. C. Martins1; 2, M. Mayor3, C. Melo5, M. Oshagh1; 2, F. Pepe3, D. Queloz3; 9, A. Santerne1, D. Ségransan3, A. Sozzetti7, S. G. Sousa1; 2; 6, and S. Udry3 1 Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 2 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre, 4169-007 Porto, Portugal 3 Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, CH-1290 Sauverny, Switzerland 4 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA 5 European Southern Observatory, Casilla 19001, Santiago, Chile 6 Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain 7 INAF - Osservatorio Astrofisico di Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy 8 Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388, Marseille, France 9 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK Received XXX; accepted XXX ABSTRACT Context. The search for planets orbiting metal-poor stars is of uttermost importance for our understanding of the planet formation models. However, no dedicated searches have been conducted so far for very low mass planets orbiting such objects. -
Star Formation Relations and CO Sleds Across the J-Ladder and Redshift 3 on the ESA Herschel Space Observatory20 (Pilbratt Et Al
Draft version July 17, 2014 Preprint typeset using LATEX style emulateapj v. 5/2/11 STAR FORMATION RELATIONS AND CO SPECTRAL LINE ENERGY DISTRIBUTIONS ACROSS THE J-LADDER AND REDSHIFT T. R. Greve1, I. Leonidaki2, E. M. Xilouris2, A. Weiß3, Z.-Y. Zhang4,5, P. van der Werf6, S. Aalto7, L. Armus8, T. D´ıaz-Santos8, A.S. Evans9,10, J. Fischer11, Y. Gao12, E. Gonzalez-Alfonso´ 13, A. Harris14, C. Henkel3, R. Meijerink6,15, D. A. Naylor16 H. A. Smith17 M. Spaans15 G. J. Stacey18 S. Veilleux14 F. Walter19 Draft version July 17, 2014 ABSTRACT 0 We present FIR[50 − 300 µm]−CO luminosity relations (i.e., log LFIR = α log LCO + β) for the full CO rotational ladder from J = 1 − 0 up to J = 13 − 12 for a sample of 62 local (z ≤ 0:1) (Ultra) 11 Luminous Infrared Galaxies (LIRGs; LIR[8−1000 µm] > 10 L ) using data from Herschel SPIRE-FTS and ground-based telescopes. We extend our sample to high redshifts (z > 1) by including 35 (sub)- millimeter selected dusty star forming galaxies from the literature with robust CO observations, and sufficiently well-sampled FIR/sub-millimeter spectral energy distributions (SEDs) so that accurate FIR luminosities can be deduced. The addition of luminous starbursts at high redshifts enlarge the range of the FIR−CO luminosity relations towards the high-IR-luminosity end while also significantly increasing the small amount of mid-J/high-J CO line data (J = 5 − 4 and higher) that was available prior to Herschel. This new data-set (both in terms of IR luminosity and J-ladder) reveals linear FIR−CO luminosity relations (i.e., α ' 1) for J = 1 − 0 up to J = 5 − 4, with a nearly constant normalization (β ∼ 2). -
![GRB 190114C: an Upgraded Legend Arxiv:1901.07505V2 [Astro-Ph.HE] 25 Mar 2019](https://docslib.b-cdn.net/cover/9296/grb-190114c-an-upgraded-legend-arxiv-1901-07505v2-astro-ph-he-25-mar-2019-509296.webp)
GRB 190114C: an Upgraded Legend Arxiv:1901.07505V2 [Astro-Ph.HE] 25 Mar 2019
GRB 190114C: An Upgraded Legend Yu Wang1;2, Liang Li 1, Rahim Moradi 1;2, Remo Ruffini 1;2;3;4;5;6 1ICRANet, P.zza della Repubblica 10, 65122 Pescara, Italy. 2ICRA and Dipartimento di Fisica, Sapienza Universita` di Roma, P.le Aldo Moro 5, 00185 Rome, Italy. 3ICRANet - INAF, Viale del Parco Mellini 84, 00136 Rome, Italy. 4Universite´ de Nice Sophia Antipolis, CEDEX 2, Grand Chateauˆ Parc Valrose, Nice, France. 5ICRANet-Rio, Centro Brasileiro de Pesquisas F´ısicas, Rua Dr. Xavier Sigaud 150, 22290–180 Rio de Janeiro, Brazil. 6ICRA, University Campus Bio-Medico of Rome, Via Alvaro del Portillo 21, I-00128 Rome, Italy. [email protected], [email protected], [email protected], ruffi[email protected] arXiv:1901.07505v2 [astro-ph.HE] 25 Mar 2019 1 Gamma-ray burst (GRB) 190114C first resembles the legendary GRB 130427A: Both are strong sources of GeV emission, exhibiting consistent GeV spectral evolution, and almost identical in detail for the morphology of light-curves in X-ray, gamma-ray and GeV bands, inferring a standard system with differ- ent scales. GRB 190114C is richer than GRB 130427A: a large percentage of ∼ 30% energy is thermal presenting in the gamma-ray prompt emission, mak- ing it as one of the most thermal-prominent GRBs; Moreover, GRB 190114C extends the horizon of GRB research, that for the first time the ultra-high energy TeV emission (> 300 GeV) is detected in a GRB as reported by the MAGIC team. Furthermore, GRB 190114C urges us to revisit the traditional theoretical framework, since most of the GRB’s energy may emit in the GeV and TeV range, not in the conventional MeV range. -
Stellar Clusters in Dwarf Galaxies
A&A 448, 471–478 (2006) Astronomy DOI: 10.1051/0004-6361:20052949 & c ESO 2006 Astrophysics Stellar clusters in dwarf galaxies L. Vanzi1 and M. Sauvage2 1 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile e-mail: [email protected] 2 CEA/DSM/DAPNIA/Service d’Astrophysique – UMR AIM, CE Saclay, 91191 Gif-sur-Yvette Cedex, France e-mail: [email protected] Received 28 February 2005 / Accepted 13 October 2005 ABSTRACT We present new observations in the Ks (2.2 µm) and L (3.7 µm) infrared bands of a sample of blue dwarf galaxies with the larger aim of studying the population of massive stellar clusters, the occurrence of dust-embedded stellar clusters, and their properties. All Ks images show a rich population of clusters, but only a small fraction of them is bright in L.MostL sources have radio counterparts. We derived the luminosity function in Ks for the galaxies IC 4661 and NGC 5408, finding both to be consistent with those of similar galaxies. We also compared the number of clusters and their luminosities with the star-formation rate of the host galaxies and found no compelling evidence of correlation. We conclude that young clusters and embedded clusters are a common feature of blue dwarf galaxies and possibly of galaxies in general, we suggest that their occurrence is due to purely statistical effects rather than a phenomenon related to specific physical conditions. In this sense we expect these objects to be abundant at high red-shift. Key words. galaxies: dwarf – galaxies: starburst – galaxies: star clusters 1. -
Decoding the Radial Velocity Variations of HD41248 with ESPRESSO
Astronomy & Astrophysics manuscript c ESO 2019 November 27, 2019 Decoding the radial velocity variations of HD41248 with ESPRESSO J. P. Faria1, V. Adibekyan1, E. M. Amazo-Gómez2; 3, S. C. C. Barros1, J. D. Camacho1; 4, O. Demangeon1, P. Figueira5; 1, A. Mortier6, M. Oshagh3; 1, F. Pepe7, N. C. Santos1; 4, J. Gomes da Silva1, A. R. Costa Silva1; 8, S. G. Sousa1, S. Ulmer-Moll1; 4, and P. T. P. Viana1 1 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal 2 Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany 3 Institut für Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, D-37077, Göttingen, Germany 4 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua Campo Alegre, 4169-007 Porto, Portugal 5 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile 6 Astrophysics Group, Cavendish Laboratory, University of Cambridge, J.J. Thomson Avenue, Cambridge CB3 0HE, UK 7 Observatoire Astronomique de l’Université de Genève, 51 chemin des Maillettes, 1290, Versoix, Switzerland 8 University of Hertfordshire, School of Physics, Astronomy and Mathematics, College Lane Campus, Hatfield, Hertfordshire, AL10 9AB, UK. Received July 26, 2019; accepted November 21, 2019 ABSTRACT Context. Twenty-four years after the discoveries of the first exoplanets, the radial-velocity (RV) method is still one of the most productive techniques to detect and confirm exoplanets. But stellar magnetic activity can induce RV variations large enough to make it difficult to disentangle planet signals from the stellar noise. -
Luglio – Settembre 2017
Raccolta di Flash news dal sito www.ilcosmo.net Luglio – Settembre 2017 Mappa di tutti gli elementi noti che formano i detriti spaziali intorno alla Terra. Questa raccolta consente l’archiviazione personale di tutte le Flash news comparse sulla homepage del nostro sito nel periodo sopra indicato. Non vi sono ulteriori commenti alle notizie. Sono impaginate in ordine cronologico di uscita. La redazione. Assemblato da Luigi Borghi. Associazione Culturale “Il C.O.S.MO.” (Circolo di Osservazione Scientifico-tecnologica di Modena); C.F.:94144450361 pag: 1 di 50 Questa raccolta, le copie arretrate, i suoi articoli, non possono essere duplicati e commercializzati. È vietata ogni forma di riproduzione, anche parziale, senza l’autorizzazione scritta del circolo “Il C.O.S.Mo”. La loro diffusione all’esterno del circolo e’ vietata. Può essere utilizzata solo dai soci per scopi didattici. - Costo: Gratuito sul WEB per i soci . Raccolta di Flash news dal sito www.ilcosmo.net 1/7/2017 - Il robot che pulirà lo spazio. Sono parecchi anni che gli scienziati e le università di tutto il mondo cercano di risolvere questo enorme problema della sicurezza del volo spaziale: l’accumulo di detriti su orbite operative è potenzialmente devastante per qualsiasi tipo di veicolo spaziale, dai satelliti operativi alle missione con astronauti ed alla ISS. Che non sia un problema facile lo si evince dalla velocità di questi “proiettili” che si aggira sui 28.000 km orari e oltre, dalla impossibilità di identificarne la composizione e dalla impssibilità di determinare i punti di presa di oggetti che, nella maggior parte dei casi, sono pure in rapida rotazione su se stessi. -
Neutral Hydrogen in Nearby Dwarf Galaxies B¨Arbel S
Dwarf Galaxies: From the Deep Universe to the Present Proceedings IAU Symposium No. 344, 2018 c 2018 International Astronomical Union K. McQuinn & S. Stierwalt, eds. DOI: 00.0000/X000000000000000X Neutral Hydrogen in Nearby Dwarf Galaxies B¨arbel S. Koribalski CSIRO Astronomy and Space Science, Australia Telescope National Facility PO Box 76, Epping, NSW 1710, Australia email: [email protected] Abstract. Here I briefly highlight our studies of the gas content, kinematics and star formation in nearby dwarf galaxies (D < 10 Mpc) based on the `Local Volume H i Survey' (LVHIS, Koribalski et al. 2018), which was conducted with the Australia Telescope Compact Array (ATCA). The LVHIS sample consists of nearly 100 galaxies, including new discoveries, spanning a large diversity in size, shape, mass and degree of peculiarity. The hydrogen properties of dwarf galaxies in two nearby groups, Sculptor and CenA / M83, are analysed and compared with many rather isolated dwarf galaxies. Around 10% of LVHIS galaxies are transitional or mixed-type dwarf galaxies (dIrr/dSph), the formation of which is explored. | I also provide a brief update on WALLABY Early Science, where we focus on studying the H i properties of galaxies as a function of environment. WALLABY (Dec < +30 degr, z < 0:26) is conducted with the Australian SKA Pathfinder (ASKAP), a ∼6-km diameter array of 36 × 12-m dishes, each equipped with wide-field (30 sq degr) Chequerboard Phased Array Feeds. Keywords. galaxies: kinematics and dynamics | galaxies: structure | radio lines: galaxies | surveys 1. LVHIS { The Local Volume H i Survey The LVHIS project provides high-resolution H i spectral line and 20-cm radio contin- uum data products for nearly 100 nearby galaxies, based on over 2500 hours of ATCA observations. -
Downloaded From
Review HEAVY METAL RULES. I. EXOPLANET INCIDENCE AND METALLICITY Vardan Adibekyan1 ID 1 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal; [email protected] Academic Editor: name Received: date; Accepted: date; Published: date Abstract: Discovery of only handful of exoplanets required to establish a correlation between giant planet occurrence and metallicity of their host stars. More than 20 years have already passed from that discovery, however, many questions are still under lively debate: What is the origin of that relation? what is the exact functional form of the giant planet – metallicity relation (in the metal-poor regime)?, does such a relation exist for terrestrial planets? All these question are very important for our understanding of the formation and evolution of (exo)planets of different types around different types of stars and are subject of the present manuscript. Besides making a comprehensive literature review about the role of metallicity on the formation of exoplanets, I also revisited most of the planet – metallicity related correlations reported in the literature using a large and homogeneous data provided by the SWEET-Cat catalog. This study lead to several new results and conclusions, two of which I believe deserve to be highlighted in the abstract: i) The hosts of sub-Jupiter mass planets (∼0.6 – 0.9 M ) are systematically less metallic than the hosts of Jupiter-mass planets. This result might be relatedX to the longer disk lifetime and higher amount of planet building materials available at high metallicities, which allow a formation of more massive Jupiter-like planets. -
FY13 High-Level Deliverables
National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2013 (1 October 2012 – 30 September 2013) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 13 December 2013 Revised 18 September 2014 Contents NOAO MISSION PROFILE .................................................................................................... 1 1 EXECUTIVE SUMMARY ................................................................................................ 2 2 NOAO ACCOMPLISHMENTS ....................................................................................... 4 2.1 Achievements ..................................................................................................... 4 2.2 Status of Vision and Goals ................................................................................. 5 2.2.1 Status of FY13 High-Level Deliverables ............................................ 5 2.2.2 FY13 Planned vs. Actual Spending and Revenues .............................. 8 2.3 Challenges and Their Impacts ............................................................................ 9 3 SCIENTIFIC ACTIVITIES AND FINDINGS .............................................................. 11 3.1 Cerro Tololo Inter-American Observatory ....................................................... 11 3.2 Kitt Peak National Observatory ....................................................................... 14 3.3 Gemini Observatory ........................................................................................ -
The Hot R Coronae Borealis Star DY Centauri Is a Binary
To appear in ApJ The hot R Coronae Borealis star DY Centauri is a binary N. Kameswara Rao1,2, David L. Lambert2, D. A. Garc´ıa-Hern´andez3,4, C. Simon Jeffery5, Vincent M. Woolf6 and Barbara McArthur2 ABSTRACT The remarkable hot R Coronae Borealis star DY Cen is revealed to be the first and only binary system to be found among the R Coronae Borealis stars and their likely relatives, including the Extreme Helium stars and the hydrogen-deficient carbon stars. Radial velocity determinations from 1982-2010 have shown DY Cen is a single-lined spectroscopic binary in an eccentric orbit with a period of 39.67 days. It is also one of the hottest and most H-rich member of the class of RCB stars. The system may have evolved from a common-envelope to its current form. Subject headings: Stars: variables: general — binaries: general — Stars: evo- lution — white dwarfs — Stars: chemically peculiar — Stars: individual: (DY Cen) 1. Introduction DY Centauri may be a remarkable member of the remarkable class of R Coronae Bo- realis (RCB) stars. RCB stars are a rare class of peculiar variable stars with two principal arXiv:1210.4199v2 [astro-ph.SR] 30 Oct 2012 and defining characteristics: (i) RCBs exhibit a propensity to fade at unpredictable times 1543, 17th Main, IV Sector, HSR Layout, Bangalore 560102, India; [email protected] 2The W.J. McDonald Observatory, University of Texas, Austin, TX 78712-1083, USA; [email protected] 3Instituto de Astrof´ısica de Canarias, C/ Via L´actea s/n, 38200 La Laguna, Spain; [email protected] 4Departamento de Astrof´ısica, Universidad de La Laguna (ULL), E-38205 La Laguna, Spain 5Armagh Observatory, College Hill, Armagh, N. -
Monte Carlo Simulations of GRB Afterglows
ABSTRACT WARREN III, DONALD CAMERON. Monte Carlo Simulations of Efficient Shock Acceleration during the Afterglow Phase of Gamma-Ray Bursts. (Under the direction of Donald Ellison.) Gamma-ray bursts (GRBs) signal the violent death of massive stars, and are the brightest ex- plosions in the Universe since the Big Bang itself. Their afterglows are relics of the phenomenal amounts of energy released in the blast, and are visible from radio to X-ray wavelengths up to years after the event. The relativistic jet that is responsible for the GRB drives a strong shock into the circumburst medium that gives rise to the afterglow. The afterglows are thus intimately related to the GRB and its mechanism of origin, so studying the afterglow can offer a great deal of insight into the physics of these extraordinary objects. Afterglows are studied using their photon emission, which cannot be understood without a model for how they generate cosmic rays (CRs)—subatomic particles at energies much higher than the local plasma temperature. The current leading mechanism for converting the bulk energy of shock fronts into energetic particles is diffusive shock acceleration (DSA), in which charged particles gain energy by randomly scattering back and forth across the shock many times. DSA is well-understood in the non-relativistic case—where the shock speed is much lower than the speed of light—and thoroughly-studied (but with greater difficulty) in the relativistic case. At both limits of speed, DSA can be extremely efficient, placing significant amounts of energy into CRs. This must, in turn, affect the structure of the shock, as the presence of the CRs upstream of the shock acts to modify the incoming plasma flow. -
Dust Production 680-850 Million Years After the Big Bang
Astronomy & Astrophysics manuscript no. ms c ESO 2018 July 12, 2018 Dust production 680–850 million years after the Big Bang Michał J. Michałowski ⋆ SUPA , Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK, [email protected] Received 12 January 2015; accepted 23 March 2015 ABSTRACT Dust plays an important role in our understanding of the Universe, but it is not obvious yet how the dust in the distant universe was formed. I derived the dust yields per asymptotic giant branch (AGB) star and per supernova (SN) required to explain dust masses of galaxies at z = 6.3–7.5 (680–850 million years after the Big Bang) for which dust emission has been detected (HFLS3 at z = 6.34, ULAS J1120+0641 at z = 7.085, and A1689-zD1 at z = 7.5), or unsuccessfully searched for. I found very high required yields, implying that AGB stars could not contribute substantially to dust production at these redshifts, and that SNe could explain these dust masses, but only if they do not destroy most of the dust they form (which is unlikely given the upper limits on the SN dust yields derived for galaxies where dust is not detected). This suggests that the grain growth in the interstellar medium is likely required at these early epochs. Key words. stars: AGB and post-AGB – supernovae: general – dust, extinction – galaxies: high-redshift – galaxies: ISM – quasars: general 1. Introduction Theoretical models predict that a SN can produce at most ∼ 1.3 M⊙ of dust (Todini & Ferrara 2001; Dust plays an important role in our understanding of the Nozawa et al.