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Estimating the Parameters of Globular Cluster M 30 (NGC 7099) from Time-Series Photometry
Astronomy & Astrophysics manuscript no. ngc7099 c ESO 2018 September 23, 2018 Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry⋆,⋆⋆ N. Kains1, D. M. Bramich1, A. Arellano Ferro2, R. Figuera Jaimes1,3, U. G. Jørgensen4,5, S. Giridhar6 and K.A. Alsubai7, J. M. Andersen8,5, V. Bozza9,10, P. Browne3, M. Burgdorf11, S. Calchi Novati9,12, Y. Damerdji13, C. Diehl14,15, P. Dodds3, M. Dominik3,⋆⋆⋆, A. Elyiv13,16, X.-S. Fang17,18, E. Giannini14, S.-H. Gu17,18, S. Hardis4, K. Harpsøe4,5, T.C. Hinse19,4, A. Hornstrup20, M. Hundertmark3, J. Jessen-Hansen21, D. Juncher4,5, E. Kerins22, H. Kjeldsen21, H. Korhonen4,5, C. Liebig3, M. N. Lund21, M. Lundkvist21, L. Mancini23, R. Martin24, M. Mathiasen4, M.T. Penny25, M. Rabus26, S. Rahvar27,28, D. Ricci29,13, K. Sahu30, G. Scarpetta9,31, J. Skottfelt4,5, C. Snodgrass32, J. Southworth33, J. Surdej13, J. Tregloan-Reed33, C. Vilela33, O. Wertz13, and A. Williams24 (The MiNDSTEp consortium) (Affiliations can be found after the references) Received ... ; accepted ... Abstract Aims. We present the analysis of 26 nights of V and I time-series observations from 2011 and 2012 of the globular cluster M 30 (NGC 7099). We used our data to search for variable stars in this cluster and refine the periods of known variables; we then used our variable star light curves to derive values for the cluster’s parameters. Methods. We used difference image analysis to reduce our data to obtain high-precision light curves of variable stars. We then estimated the cluster parameters by performing a Fourier decomposition of the light curves of RR Lyrae stars for which a good period estimate was possible. -
ACE Mentor Program of Greater NY Participating Schools 2019-20
ACE Mentor Program of Greater NY Participating Schools 2019-20 A.Phillip Randolph Campus High School Channel View School for Research Hendrick Hudson High School Abraham Clark High School Chelsea CTE High School High School for Construction Trades, Engineering, Abraham Lincoln High School Church of God Christian Academy and Architecture Academy of American Studies City College Academy of the Arts High School for Contemporary Arts Academy of Finance and Enterprises City Polytechnic High School of Engineering, High School for Environmental Studies Academy of Urban Planning and Engineering Architecture, and Technology High School for Health Professions and Human All City Leadership Academy Civic Leadership Academy Services All Hallows High School Clarkstown High School North High School for Math, Science and Engineering and All Hallows Institute Clarkstown High School South City College of NY Archbishop Molloy High School Cold Spring Harbor High School High School of Arts and Technology Archbishop Stepinac High School College of Staten Island High School for High School of Computers and Technology Art & Design High School International Studies High School of Economics and Finance Avenues: The World School Columbia Secondary School for Math, Science, and High School of Telecommunications Arts and Aviation High School Engineering Technology Baldwin Senior High School Community Health Academy of the Heights Hillcrest High School Bard High School Early College Manhattan Cristo Rey New York High School Hillside Arts and Letters Academy Bard High School Early College Queens Croton Harmon High School Holy Cross High School Baruch College Campus Curtis High School Holy Trinity Diocesan High School Bayside High school Davis Renov Stahler Yeshiva High School Horace Greeley High School Beacon School Democracy Prep Charter High School Horace Mann School Bedford Academy High School Digital Tech High School Humanities Prep High School Benjamin Banneker Academy Dix Hills High School West Hunter College High School Benjamin N. -
A Deeper Look at Leo Iv: Star Formation History and Extended Structure
A DEEPER LOOK AT LEO IV: STAR FORMATION HISTORY AND EXTENDED STRUCTURE The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Sand, David J., Anil Seth, Edward W. Olszewski, Beth Willman, Dennis Zaritsky, and Nitya Kallivayalil. “A DEEPER LOOK AT LEO IV: STAR FORMATION HISTORY AND EXTENDED STRUCTURE.” The Astrophysical Journal 718, no. 1 (July 1, 2010): 530–542. © 2010 The American Astronomical Society As Published http://dx.doi.org/10.1088/0004-637x/718/1/530 Publisher IOP Publishing Version Final published version Citable link http://hdl.handle.net/1721.1/95689 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The Astrophysical Journal, 718:530–542, 2010 July 20 doi:10.1088/0004-637X/718/1/530 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. A DEEPER LOOK AT LEO IV: STAR FORMATION HISTORY AND EXTENDED STRUCTURE∗ David J. Sand1,5, Anil Seth1, Edward W. Olszewski2, Beth Willman3, Dennis Zaritsky2, and Nitya Kallivayalil4,6 1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA 02138, USA; [email protected] 2 Steward Observatory, University of Arizona, Tucson, AZ 85721, USA 3 Haverford College, Department of Astronomy, 370 Lancaster Avenue, Haverford PA 19041, USA 4 MIT Kavli Institute for Astrophysics & Space Research, 70 Vassar Street, Cambridge, MA 02139, USA Received 2009 November 26; accepted 2010 May 24; published 2010 July 1 ABSTRACT We present MMT/Megacam imaging of the Leo IV dwarf galaxy in order to investigate its structure and star formation history, and to search for signs of association with the recently discovered Leo V satellite. -
Variable Stars in the Globular Cluster M 13 Ability of V7 Was Confirmed by Shapley (1915B)
Astronomy & Astrophysics manuscript no. h3895 October 23, 2018 (DOI: will be inserted by hand later) Variable stars in the globular cluster M 13 G. Kopacki, Z. Kołaczkowski, and A. Pigulski Wrocław University Observatory, Kopernika 11, 51-622 Wrocław, Poland Received .....; accepted ..... Abstract. Results of a search for variable stars in the central region of the globular cluster M 13 are presented. Prior to this study, 36 variable and suspected variable stars were known in this cluster (Osborn 2000; Clement et al. 2001). Of these stars, five were not observed by us. We find v3, v4, v10, v12, and v13 to be constant in light. Surprisingly, only two out of the ten variable star candidates of Kadla et al. (1980) appear to be variable. Both are RRc variables. Additionally, three RR Lyrae stars and one SX Phoenicis variable are discovered. Three close frequencies are detected for an RRc star v36. It appears that this variable is another multi-periodic RR Lyrae star pulsating in non-radial modes. Light curves of the three known BL Herculis stars and all known RR Lyrae stars are presented. The total number of known RR Lyrae stars in M 13 is now nine. Only one is an RRab star. The mean period of RRc variables amounts to 0.36 ± 0.05 d, suggesting that M 13 should be included in the group of Oosterhoff type II globular clusters. Mean V magnitudes and ranges of variation are derived for seven RR Lyrae and three BL Herculis variables. Almost all observed bright giants show some degree of variability. -
Blications of the Astronomical Society of the Pacific, 115:755–760, 2003 June ᭧ 2003
Publications of the Astronomical Society of the Pacific, 115:755–760, 2003 June ᭧ 2003. The Astronomical Society of the Pacific. All rights reserved. Printed in U.S.A. Differential Time-Series CCD Photometry of BL Camelopardalis Revisited Chulhee Kim Department of Earth Science Education, Chonbuk National University, Korea; [email protected] and Y.-B. Jeon and S.-L. Kim Department of Earth Science Education, Chonbuk National University, Korea; and Korea Astronomy Observatory, Yeoungcheon 770-880, Korea Received 2003 January 11; accepted 2003 February 28 ABSTRACT. New differential time-series observations of BL Camelopardalis were secured using B and V filters. It was confirmed that BL Cam is an optical double star. Differential magnitudes were obtained through a photometric profile reduction procedure to eliminate the influence of a faint adjacent star. Variations inO Ϫ C values for light maxima were investigated. We found that the parabolic period variation was recently reversed. The periods of BL Cam were investigated, and five frequencies were determined using Fourier analysis. We also investigated the relationship between metallicities and period ratios, and we compared the theoretical and observational relationships. It was found that the theoretical relationship is better than the observational one for BL Cam. 1. INTRODUCTION been discovered. Interestingly, three of the 12 are double-mode pulsators (McNamara 1997; Martin & Rodrı´guez 1995). BL Camelopardalis ( p 03h47m19s, p ϩ63Њ22 7 a d BL Cam was first discovered by Giclas, Burnham, & Thomas [J2000.0],V p 13.10 ,V p 0.33 mag) was classified as an D (1970) as a possible white dwarf candidate. -
NEW SX PHOENICIS VARIABLES in the GLOBULAR CLUSTER NGC 48331 Andrew N
Journal of the Southeastern Association for Research in Astronomy, 6, 00-00, November 8, 2018 c 2010. Southeastern Association for Research in Astronomy. All rights reserved. NEW SX PHOENICIS VARIABLES IN THE GLOBULAR CLUSTER NGC 48331 Andrew N. Darragh and Brian W. Murphy Department of Physics and Astronomy, Butler University, Indianapolis, IN, 46208 & SARA ABSTRACT We report the discovery of 6 SX Phoenicis stars in the southern globular cluster NGC 4833. Images were obtained from January through June 2011 with the Southeastern Association for Research in Astronomy 0.6 meter telescope located at Cerro Tololo Interamerican Observatory. The image sub- traction method of Alard & Lupton (1998) was used to search for variable stars in the cluster. We confirmed 17 previously cataloged variables by Demers & Wehlau(1977). In addition to the previously known variables we have identified 10 new variables. Of the total number of confirmed variables in our 10×10 arcmin2 field, we classified 10 RRab variables, with a mean period of 0.69591 days, 7 RRc, with a mean period of 0.39555 days, 2 possible RRe variables with a mean period of 0.30950 days, a W Ursae Majoris contact binary, an Algol-type binary, and the 6 SX Phoenicis stars with a mean period of 0.05847 days. The periods, relative numbers of RRab and RRc variables, and Bailey diagram are indicative of the cluster being of the Oosterhoff type II. We present the phased-light curves, periods of previously known variables and the periods and classifications of the newly discovered variables, and their location on the color-magnitude diagram. -
Times of Maximum of KZ Hya from OACS -UNAH
REF-UNAH v8i2, 90-93 (2020) • DOI: Pendiente Times of maximum of KZ Hya from OACS -UNAH M. MEZA1,†, A. PINEDA2,†, C. ARGUETA1,†, Y. MENDOZA2,†, M.C. PEREIRA1,†, W. FUENTES3,†, M. INTERIANO2,† Recibido: 15 de octubre de 2020 / Aceptado: 5 de enero de 2021 A pulsating variable star is one whose brightness changes periodically 1 due to the expansion and contraction of the surface layers of the star. Facultad de Ciencias Espaciales, Universidad Several times of maximum light can be obtained in brief observations Nacional Autónoma de Honduras. of SX Phoenicis variable stars due to their short periods of pulsation (P ∼ 1:0 − 1:75 h). We report three new times of maximum light of SX 2Escuela de Física, Facultad de Ciencias, Phoenicis star KZ Hya obtained from photometric observations made on the night of April 5-6, 2019 from the Observatorio Astronómico Cen- Universidad Nacional Autónoma de Honduras. troaméricano de Suyapa (OACS) of the Universidad Nacional Autónoma de Honduras. 3Departamento de Física, Universidad Nacional Autónoma de Honduras en el Valle de Sula. Una estrella variable pulsante es una cuyo brillo cambia periódicamente debido a la expansión y contracción de las capas superficiales de la es- †Grupo de Investigación en Estrellas Pulsantes - trella. Las estrellas variables SX Phoenicis tienen periodos de pulsación UNAH. [email protected] cortos (P ∼ 1:0 − 1:75 h) por lo que se pueden obtener varios tiempos de máximo en observaciones cortas. Se reportan tres tiempos de máximo para la estrella SX Phoenicis KZ Hya, obtenidos a partir de observa- ciones fotométricas hechas en la noche del 5-6 de abril de 2019 desde Special Thanks el Observatorio Astronómico Centroaméricano de Suyapa (OACS) de la UNAH. -
New York State Principals New York State's High Schools, Middle Schools and Elementary Schools an Open Letter of Concern Regar
New York State Principals New York State’s High Schools, Middle Schools and Elementary Schools An Open Letter of Concern Regarding New York State’s APPR Legislation for the Evaluation of Teachers and Principals www.newyorkprincipals.org Over the past year, New York State has implemented dramatic changes to its schools. As building principals, we recognize that change is an essential component of school improvement. We continually examine best practices and pursue the most promising research-based school improvement strategies. We are very concerned, however, that at the state level change is being imposed in a rapid manner and without high-quality evidentiary support. Our students, teachers and communities deserve better. They deserve thoughtful reforms that will improve teaching and learning for all students. It is in this spirit that we write this letter, which sets forth our concerns and offers a path forward. We believe that it is our ethical obligation as principals to express our deep concerns about the recently implemented Annual Professional Performance Review (APPR) regulations. These regulations are seriously flawed, and our schools and students will bear the brunt of their poor design. Below we explain why we are opposed to APPR as it is presently structured. Background In May 2010, the New York State Legislature—in an effort to secure federal Race to the Top funds— approved an amendment to Educational Law 3012-c regarding the Annual Professional Performance Review (APPR) of teachers and principals. The new law states that beginning September 2011, all teachers and principals will receive a number from 0-100 to rate their performance. -
1997 Highlights
from the 1997 Annual Report research. The projects and thinking I have outlined are all essential for our research insti- tution to remain dynamic. At the same time, we must make sure that our scientists are supported to the fullest extent possible and that the research remains of the highest pos- sible quality, in the new academic style. HIGHLIGHTS OF THE YEAR Research Highlights Cancer Genetics and Cell Division In March, Cold Spring Harbor Laboratory (CSHL) scientists Michael Wigler and Clifford Yen with colleague Ramon Parsons, M.D., Ph.D., of the Herbert Irving Comprehensive Cancer Center and Columbia-Presbyterian Medical Center, announced the discovery of a tumor suppressor gene, which they named PTEN. The gene appears to be altered in a large percentage of brain, breast, and prostate cancers, and evidence suggests that loss of PTEN affects the way a benign tumor becomes malignant. Unlike mutations of genes such as hMSH2 and BRCA1, which were found in people who have hered- itary predispositions to cancer, PTEN was discovered by analyzing the more com- mon sporadic cancers. More than 80% of all cases of cancer are sporadic, mean- ing that they have no obvious hereditary contribution. PTEN received its name because of its similarity to phosphatases and tensin. The similarity between PTEN and protein phosphatases, which remove phosphates from proteins, is significant because many oncogenes—genes that help to trans- form normal cells into cancer cells—encode tyrosine kinases, which add phos- phates to proteins. Tensin is part of a complex of proteins that sits below the cell surface and controls cell shape. -
Summer 2009 Issue No
“Lies! Lies! All of It, Lies!” Summer 2009 Issue No. 22 JHS Classes of ‘71, ‘72, ‘73 Thirderly Online Newsletter Welcome to this, the 22nd news- letter of the JHS classes of ‘71, Official Propaganda Tool of ‘71, ‘72, ‘73 Jericho High Alumni ‘72, and ‘73, and friends. ReunionIn this Update issue: 1 In publishing, they say that if you want Yearbook to Facebook 12 Lori Light, Lori Small Cohan, to attract readers, Arnold Holtz, Mitchell Bau- 2 moel , Roslyn Appelbaum, just put a cute ‘n Ellen Tillman, Alan Abbadan- cuddly kitten on gelo, Anne K. Havrilla your cover. We’ve Nooz About Yooz 3 gone one better … Mr. Bob Hoffman, Hall of Fame Induction, more In Tribute 45 “Pets: Man’s Deirdre Rasulo Catch Up With … 67 Best Friend”* Caren Kushner Gottesman Takin’ Care of Bidness — 9 * And in Your Case, Jerichonians at Work 11 That’s Understand- Jane Altvater Duda 12 able! Cartoons by Dan Clurman 12 First Person Singular 13 Mindy Wertheimer Pix of Your Pets Everything You Ever Wanted 1517 Beginning on page 24 to Know About: Jan Millner Everything You Ever Wanted 20 to Know About: Lisa Stewart Discounted Advance Jacobs and Beth Stewart 17 Reunion Tix Now On Sale Cover Story 1924 Pets: Man’s (and Woman’s) 25 Advance tickets for the October 9, 2010, “Inter- Best Friend, featuring Ellen galactic Space Party” at Milleridge Cottage went on Jankowitz, Bonnie Colgan, sale beginning July 4. From then until February 9, Diane Freedman, Randy San 28 2010, admission is $100 per adult — a savings of Antonio, Amy Lubow, more $25 per ticket. -
Estudo Fotométrico E Descoberta De Novas Estrelas Variáveis Nos
Elizandra Martinazzi Estudo fotom´etrico e descoberta de novas estrelas vari´aveis nos Aglomerados Globulares NGC6397 e NGC288 Porto Alegre 2016 UNIVERSIDADE FEDERAL DO RIO GRANDE DO SUL PROGRAMA DE POS-GRADUAC¸´ AO˜ EM F´ISICA Estudo fotom´etrico e descoberta de novas estrelas vari´aveis nos Aglomerados Globulares NGC6397 e NGC288 Elizandra Martinazzi Tese de doutorado realizado sob ori- enta¸c˜ao do Prof. Dr. Kepler de Souza Oliveira Filho, co-orienta¸c˜ao do Prof. Dr. Jos´eEduardo da Silveira Costa e apresen- tado ao curso de P´os-Gradua¸c˜ao em F´ısica em preenchimento dos requisitos para ob- ten¸c˜ao do t´ıtulo de Doutor em F´ısica. Porto Alegre, RS, Brasil 2016. ⋆ Trabalho financiado pela CAPES Agradecimentos Agrade¸co de forma geral a todos que colaboraram para a realiza¸c˜ao deste trabalho; em particular, ao meu orientador professor Dr. Kepler de Souza Oliveira Filho pelo est´ımulo, compreens˜ao e companheirismo para realiza¸c˜ao deste trabalho, assim como meu coorientador professor Dr. Jos´eEduardo da Silveira Costa; Aos meus pais e ao meu irm˜ao, pelo apoio e compreens˜ao da importˆancia de minha forma¸c˜ao acadˆemica; A todos os professores e colegas do Departamento de Astronomia, A todos os meus amigos, colegas e alunos que de alguma maneira contribu´ıram com este trabalho. I Resumo Neste trabalho, estudamos dois aglomerados globulares, o NGC 6397 com m´odulo de distˆancia (m − M) = 12,03 ± 0,06 mag e o NGC288 com m´odulo de distˆancia (m − M) = 14,57 ± 0,08 mag. -
Discrete Scale Relativity and Sx Phoenicis Variable Stars
DISCRETE SCALE RELATIVITY AND SX PHOENICIS VARIABLE STARS Robert L. Oldershaw 12 Emily Lane Amherst, MA 01002 USA [email protected] Abstract: Discrete Scale Relativity proposes a new symmetry principle called discrete cosmological self-similarity which relates each class of systems and phenomena on a given Scale of nature’s discrete cosmological hierarchy to the equivalent class of analogue systems and phenomena on any other Scale. The new symmetry principle can be understood in terms of discrete scale invariance involving the spatial, temporal and dynamic parameters of all systems and phenomena. This new paradigm predicts a rigorous discrete self-similarity between Stellar Scale variable stars and Atomic Scale excited atoms undergoing energy-level transitions and sub- threshold oscillations. Previously, methods for demonstrating and testing the proposed symmetry principle have been applied to RR Lyrae, δ Scuti and ZZ Ceti variable stars. In the present paper we apply the same analytical methods and diagnostic tests to a new class of variable stars: SX Phoenicis variables. Double-mode pulsators are shown to provide an especially useful means of testing the uniqueness and rigor of the conceptual principles and discrete self-similar scaling of Discrete Scale Relativity. 1 I. Introduction a. Preliminary discussion of discrete cosmological self-similarity The arguments presented below are based on the Self-Similar Cosmological Paradigm (SSCP)1- 6 which has been developed over a period of more than 30 years, and can be unambiguously tested via its definitive predictions 1,4 concerning the nature of the galactic dark matter. Briefly, the discrete self-similar paradigm focuses on nature’s fundamental organizational principles and symmetries, emphasizing nature’s intrinsic hierarchical organization of systems from the smallest observable subatomic particles to the largest observable superclusters of galaxies.