DOCSLIB.ORG

Detection of White Dwarf Companions to Blue Stragglers in the Open

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Detection of White Dwarf Companions to Blue Stragglers in the Open Draft version May 6, 2018 A Preprint typeset using LTEX style emulateapj v. 5/2/11 DETECTION OF WHITE DWARF COMPANIONS TO BLUE STRAGGLERS IN THE OPEN CLUSTER NGC 188: DIRECT EVIDENCE FOR RECENT MASS TRANSFER Natalie M. Gosnell1, Robert D. Mathieu1, Aaron M. Geller2,3, Alison Sills4, Nathan Leigh5,6, Christian Knigge7 Draft version May 6, 2018 ABSTRACT Several possible formation pathways for blue straggler stars have been developed recently, but no one pathway has yet been observationally confirmed for a specific blue straggler. Here we report the first findings from a Hubble Space Telescope ACS/SBC far-UV photometric program to search for white dwarf companions to blue straggler stars. We find three hot and young white dwarf companions to blue straggler stars in the 7-Gyr open cluster NGC 188, indicating that mass transfer in these systems ended less than 300 Myr ago. These companions are direct and secure observational evidence that these blue straggler stars were formed through mass transfer in binary stars. Their existence in a well-studied cluster environment allows for observational constraints of both the current binary system and the progenitor binary system, mapping the entire mass transfer history. Subject headings: open clusters and associations: individual (NGC 188) — binaries: spectroscopic — blue stragglers — white dwarfs — ultraviolet: stars 1. INTRODUCTION eccentricity distributions provide clues to their formation Blue straggler stars (BSSs), originally defined to be histories (Mathieu & Geller 2009, 2013). Of the 16 NGC anomalous stars more luminous and bluer than the main 188 BSSs in binaries, all but three have orbital periods sequence (MS) of a star cluster, are now known to near 1000 days. Statistical analysis of their secondary- be present in open star clusters (Johnson & Sandage mass distribution suggests that the companions to these 1955), globular clusters (Sandage 1953; Ferraro et al. BSSs have masses around 0.5 M⊙ (Geller & Mathieu 1999), the Galactic field (Preston & Sneden 2000), and 2011). Such masses suggest white dwarf (WD) compan- dwarf spheroidal galaxies (Momany et al. 2007). They ions, whose presence would indicate mass transfer as the define an alternative stellar evolution path, yet not a dominant BSS formation mechanism in NGC 188. rare one; BSSs comprise 25% of the evolved popula- The presence of a WD is detectable as an excess of tion in NGC 188 (Geller et al. 2008). Even so, the UV emission above the expected emission from a BSS formation of BSSs has been a puzzle for almost six alone. In this Letter we present the first results from decades. Recent work has identified several possible a Hubble Space Telescope (HST ) program searching for formation pathways, including mergers in hierarchical WD companions to the BSSs in NGC 188. We outline triples (Perets & Fabrycky 2009), collisions during dy- the observational design in § 2, the WD detections in namical encounters (Knigge et al. 2009; Leigh & Sills § 3, implications of these detections in § 4, mass transfer 2011), and mass transfer on the red giant branch (RGB) histories in § 5, and summarize our results in § 6. or asymptotic giant branch (AGB; Chen & Han 2008). 2. Yet no one pathway has yet been observationally con- OBSERVATIONS firmed for a specific BSS. NGC 188 contains 20 BSSs8 determined to be The open cluster NGC 188 contains one of the most three-dimensional members from radial-velocity (RV) thoroughly studied populations of BSSs in our Galaxy. and proper-motion (PM) studies (Platais et al. 2003; arXiv:1401.7670v1 [astro-ph.SR] 29 Jan 2014 Spectroscopic studies reveal that 80% of the BSSs in Geller et al. 2009). The population consists of 2 double- NGC 188 are in binaries, and their remarkable period and lined spectroscopic binaries, 14 single-lined spectroscopic binaries, and 4 stars that do not show velocity varia- This is WIYN Open Cluster Survey paper LVIII tions. In addition, there is one BSS candidate (WOCS [email protected] 1 4230) that is a PM member and velocity variable but Department of Astronomy, University of Wisconsin - Madi- son, 475 N. Charter St., Madison, WI 53706 whose rapid rotation does not permit sufficiently pre- 2 Center for Interdisciplinary Exploration and Research in As- cise velocities for a secure RV membership determina- trophysics (CIERA) and Department of Physics and Astronomy, tion. We observed the 14 single-lined binaries, the 4 Northwestern University, 2145 Sheridan Rd, Evanston, IL 60208 3 non-velocity variable BSSs, and WOCS 4230 using the Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637 Advanced Camera for Surveys (ACS) Solar Blind Chan- 4 Department of Physics and Astronomy, McMaster Univer- nel (SBC) onboard HST. The non-velocity variable BSSs sity, 1280 Main St. W, Hamilton, ON L8S 4M1, Canada may still have very wide binary companions beyond the 5 Department of Physics, University of Alberta, CCIS 4-183, Edmonton, AB T6G 2E1, Canada RV sensitivity, so they are included in our observational 6 Department of Astrophysics, American Museum of Natural History, Central Park West and 79th Street, New York, NY 8 After the HST observations we discovered a V -band photomet- 10024 ric error for WOCS 1947, previously categorized as a BSS, which 7 School of Physics and Astronomy, University of Southamp- revealed it to be a RGB star. It is no longer considered a member ton, Highfield, Southampton, SO17 IBJ, UK of the NGC 188 BSS population (Mathieu & Geller 2013). 2 GOSNELL ET AL. study. We did not observe the two double-lined BSS bi- 18 naries as they have almost equal-mass companions that 11000 13250 15500 17750 20000 are already known to not be WDs. Each BSSs was White Dwarf Temperature (K) WOCS 4540 observed in a separate visit of 2 orbits, for a total of WOCS 5379 38 orbits (GO:12492, PI: Mathieu), using the F140LP, 20 F150LP, and F165LP filters with total exposure times of WOCS 4348 2040 s, 2380 s, and 1564 s, respectively. 2.1. Aperture Photometry F150N 22 % We use the astrodrizzle routine to create master driz- 30 % zled images in each filter for each target with a result- 90 ′′ −1 99% ing pixel scale of 0.025 pixel . We carry out aperture 50% 24 70% photometry using the IRAF package daophot with an aperture radius of 6 pixels, or an angular radius of 0.15′′. We then apply an encircled energy fraction correction to 0 1 2 3 4 our count rates based on aperture photometry of nor- F150N - F165LP malized TinyTim-modeled point sources9. We apply the same drizzling routine to the TinyTim source and carry Fig. 1.— Far-UV color-magnitude diagram showing the positions out aperture photometry, from which we calculate the of WOCS 4540, 5379, and 4348, each shown with 2-sigma error fraction of flux missed by our aperture. We find and ap- bars. The grey contours show the expected density distribution of ply encircled energy corrections of 0.83, 0.84, and 0.85 for single BSSs with temperature and luminosity distributions match- F140LP, F150LP, and F165LP, respectively. We calcu- ing the BSS population in NGC 188 (Mathieu & Geller 2009). The outermost contour encompasses 99% of single BSSs. The colored late our corrected count rates by dividing the measured lines track synthetic BSS-WD pairs with increasing WD tempera- count rate by the encircled energy correction. We con- ture as indicated by the color bar. The lower and upper solid lines vert our corrected count rates to instrument fluxes using follow binaries with BSS temperatures of 6,000 K and 6,500 K, re- the conversion factors given in the ACS Data Handbook spectively (Rodr´ıguez-Merino et al. 2005). The dashed lines track constant WD temperature from 11,000 K to 20,000 K in increments (Gonzaga et al. 2013). of 1,000 K (P. Bergeron, private communication). Comparing the The nested bandpasses of the HST /ACS/SBC long- observations with the synthetic BSS-WD models we determine that pass filters provide an opportunity to isolate the all three systems have WD companions with temperatures of ap- bluest UV flux. As shown in previous studies (e.g., proximately 13,000 K and above, which corresponds to an age of Dieball et al. 2005), one can difference the count rates less than 300 Myr. from the long-pass filters to create derived narrow band- 10,000 times and synthetically observed using the syn- passes. We create the derived filters of F140N = phot package to create the density contours plotted in (F140LP−F150LP) and F150N = (F150LP−F165LP). To photometer the count rates for these derived filters Figure 1. The outermost contour contains 99% of the ex- we difference the corrected long-pass filter count rates pected single-BSS distribution. The three detected BSSs and calculate fluxes by applying conversion rates of are much brighter and bluer than the single-BSS dis- tribution; they must have an additional source of UV −17 2 −1 −1 PHOTLAMSBC/F140N = 7.0631 × 10 erg cm A˚ count emission. × −17 2 ˚−1 −1. To illustrate that the UV fluxes for these sources are PHOTLAMSBC/F150N = 6 4868 10 erg cm A count straightforwardly explained by the presence of young, hot We find the conversion rates using the IRAF package WD companions, in Figure 2 we show model spectra of synphot and the tasks calcband and bandpar. After a BSS-WD binary compared to the narrow-band pho- finding the narrow-band fluxes we calculate magnitudes tometry for each of the three sources. The WD and BSS in all filters using STMAG = −2.5 log (flux) − 21.1. components are shown in blue and red, respectively, with 10 the combined spectrum shown in grey.
Load more

Recommended publications
  • Open Cluster NGC 188 Explored with Astrosat 9 December 2020, by Tomasz Nowakowski
    Open cluster NGC 188 explored with AstroSat 9 December 2020, by Tomasz Nowakowski Discovered in 1825, NGC 188 is an open cluster in the constellation Cepheus, located some 5,400 light years away from the Earth. It has a solar metallicity, a radius of about 11.8 light years, reddening at a level of 0.036, and its age is estimated to be 7 billion years. It is one of the oldest and well studied OCs in our galaxy. In order to learn more about the member stars of NGC 188, a team of astronomers led by Sharmila Rani of the Indian Institute of Astrophysics in Bengaluru, India, has performed a photometric study of this cluster with the main goal of identifying its ultraviolet-bright stars. For this purpose, they used AstroSat's Ultraviolet Imaging Telescope (UVIT). "In this study, we present the results of the UV UVIT image of NGC 188 obtained by combining images imaging of the NGC 188 in two FUV [far-ultraviolet] in NUV (N279N) and FUV (F148W) channels. Yellow and one NUV [near-ultraviolet] ?lters using UVIT on and blue color corresponds to NUV and FUV detections, AstroSat. We characterize the UV bright stars respectively. Credit: Rani et al., 2020. identi?ed in this cluster by analysing SEDs [spectral energy distributions] to throw light on their formation and evolution," the astronomers wrote in the paper. Indian researchers have carried out ultraviolet photometric observations of an old open cluster FUV observations detected hot and bright blue known as NGC 188. Results of the study, straggler stars (BSSs), one hot subdwarf, and one conducted with the AstroSat spacecraft, provide white dwarf candidate.
    [Show full text]
  • Arxiv:1606.06587V1 [Astro-Ph.SR] 21 Jun 2016 Rpitsbitdt Elsevier to Submitted Preprint Sn MS Aao.W Bandtecutrsdsac Fro Distance Cluster’S the Obtained We Catalog
    2MASS photometry and kinematical studies of open cluster NGC 188 W. H. Elsanhourya,b1, A. A. Haroona,c, N. V. Chupinad, S. V. Vereshchagind, Devesh P. Sariyae2, R. K. S. Yadav f , Ing-Guey Jiange aAstronomy Department, National Research Institute of Astronomy and Geophysics (NRIAG) 11421, Helwan, Cairo, Egypt bPhysics Department, Faculty of Science, Northern Border University, Rafha Branch, Saudi Arabia cAstronomy Department, Faculty of Science, King Abdul Aziz University, Jeddah, Saudi Arabia dInstitute of Astronomy Russian Academy of Sciences (INASAN),48 Pyatnitskaya st., Moscow, Russia eDepartment of Physics and Institute of Astronomy, National Tsing Hua University, Hsin-Chu, Taiwan f Aryabhatta Research Institute of observational sciencES (ARIES), Manora Peak Nainital 263 002, India. Abstract In this paper, we present our results for the photometric and kinematical studies of old open cluster NGC 188. We determined various astrophysical parameters like limited radius, core and tidal radii, distance, luminosity and mass functions, total mass, relaxation time etc. for the cluster using 2MASS catalog. We obtained the cluster’s distance from the Sun as 1721 41 pc and log (age)= 9.85 0.05 at Solar metallicity. The relaxation time of the cluster is smaller± than the estimated cluster± age which suggests that the cluster is dynamically relaxed. Our results agree with the values mentioned in the literature. We also determined the clusters apex coordinates as (281◦.88, 44◦.76) using AD-diagram method. Other kinematical parameters like space velocity components,− cluster center and elements of Solar motion etc. have also been computed. Keywords: Open clusters- Color-magnitude diagram- Kinematics- AD diagram 1.
    [Show full text]
  • Batc 15 Band Photometry of the Open Cluster Ngc
    The Astronomical Journal, 150:61 (8pp), 2015 August doi:10.1088/0004-6256/150/2/61 © 2015. The American Astronomical Society. All rights reserved. BATC 15 BAND PHOTOMETRY OF THE OPEN CLUSTER NGC 188 Jiaxin Wang1,2, Jun Ma1, Zhenyu Wu1, Song Wang1, and Xu Zhou1 1 Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; [email protected] 2 University of Chinese Academy of Sciences, Beijing 10039, China Received 2015 April 2; accepted 2015 June 23; published 2015 July 24 ABSTRACT This paper presents CCD multicolor photometry for the old open cluster NGC 188. The observations were carried out as part of the Beijing–Arizona–Taiwan–Connecticut Multicolor Sky Survey from 1995 February to 2008 March, using 15 intermediate-band filters covering 3000–10000 Å. By fitting the Padova theoretical isochrones to our data, the fundamental parameters of this cluster are derived: an age of t =7.5 0.5 Gyr, a distance modulus of (mM-=)0 11.17 0.08, and a reddening of E (BV-= ) 0.036 0.010. The radial surface density profile of NGC 188 is obtained using the star count. By fitting the King model, the structural parameters of NGC 188 are derived: a core radius of Rc =¢3.80, a tidal radius of Rt =¢44.78, and a concentration parameter of a C0 ==log(RRtc ) 1.07. Fitting the mass function (MF) to a power-law function f ()mmµ , the slopes of the MFs for different spatial regions are derived. We find that NGC 188 presents a slope break in the MF.
    [Show full text]
  • Open Clusters
    Open Clusters Open clusters (also known as galactic clusters) are of tremendous importance to the science of astronomy, if not to astrophysics and cosmology generally. Star clusters serve as the "laboratories" of astronomy, with stars now all at nearly the same distance and all created at essentially the same time. Each cluster thus is a running experiment, where we can observe the effects of composition, age, and environment. We are hobbled by seeing only a snapshot in time of each cluster, but taken collectively we can understand their evolution, and that of their included stars. These clusters are also important tracers of the Milky Way and other parent galaxies. They help us to understand their current structure and derive theories of the creation and evolution of galaxies. Just as importantly, starting from just the Hyades and the Pleiades, and then going to more distance clusters, open clusters serve to define the distance scale of the Milky Way, and from there all other galaxies and the entire universe. However, there is far more to the study of star clusters than that. Anyone who has looked at a cluster through a telescope or binoculars has realized that these are objects of immense beauty and symmetry. Whether a cluster like the Pleiades seen with delicate beauty with the unaided eye or in a small telescope or binoculars, or a cluster like NGC 7789 whose thousands of stars are seen with overpowering wonder in a large telescope, open clusters can only bring awe and amazement to the viewer. These sights are available to all.
    [Show full text]
  • Caldwell Catalogue - Wikipedia, the Free Encyclopedia
    Caldwell catalogue - Wikipedia, the free encyclopedia Log in / create account Article Discussion Read Edit View history Caldwell catalogue From Wikipedia, the free encyclopedia Main page Contents The Caldwell Catalogue is an astronomical catalog of 109 bright star clusters, nebulae, and galaxies for observation by amateur astronomers. The list was compiled Featured content by Sir Patrick Caldwell-Moore, better known as Patrick Moore, as a complement to the Messier Catalogue. Current events The Messier Catalogue is used frequently by amateur astronomers as a list of interesting deep-sky objects for observations, but Moore noted that the list did not include Random article many of the sky's brightest deep-sky objects, including the Hyades, the Double Cluster (NGC 869 and NGC 884), and NGC 253. Moreover, Moore observed that the Donate to Wikipedia Messier Catalogue, which was compiled based on observations in the Northern Hemisphere, excluded bright deep-sky objects visible in the Southern Hemisphere such [1][2] Interaction as Omega Centauri, Centaurus A, the Jewel Box, and 47 Tucanae. He quickly compiled a list of 109 objects (to match the number of objects in the Messier [3] Help Catalogue) and published it in Sky & Telescope in December 1995. About Wikipedia Since its publication, the catalogue has grown in popularity and usage within the amateur astronomical community. Small compilation errors in the original 1995 version Community portal of the list have since been corrected. Unusually, Moore used one of his surnames to name the list, and the catalogue adopts "C" numbers to rename objects with more Recent changes common designations.[4] Contact Wikipedia As stated above, the list was compiled from objects already identified by professional astronomers and commonly observed by amateur astronomers.
    [Show full text]
  • Arxiv:1507.01949V1 [Astro-Ph.SR] 7 Jul 2015
    STELLAR RADIAL VELOCITIES IN THE OLD OPEN CLUSTER M67 (NGC 2682) I. MEMBERSHIPS, BINARIES, AND KINEMATICS ∗ Aaron M. Geller†,‡ Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics & Astronomy, Northwestern University, Evanston, IL 60201, USA, Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USA; [email protected] David W. Latham Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected] Robert D. Mathieu† Department of Astronomy, University of Wisconsin - Madison, WI 53706, USA; [email protected] ABSTRACT We present results from 13776 radial-velocity measurements of 1278 candidate members of the old (4 Gyr) open cluster M67 (NGC 2682). The measurements are the results of a long-term survey that includes data from seven telescopes with observations for some stars spanning over 40 years. For narrow-lined stars, radial velocities are measured with precisions ranging from about 0.1 to 0.8 km s−1. The combined stellar sample reaches from the brightest giants in the cluster down to about 4 mag- nitudes below the main-sequence turnoff (V = 16.5), covering a mass range of about 1.34 M⊙ to 0.76 M⊙. Spatially, the sample extends to a radus of 30 arcminutes (7.4 pc in projection at a distant of 850 pc or 6-7 core radii). We find M67 to have a mean radial velocity of +33.64 km s−1 (with an internal precision of ±0.03 km s−1) well separated from the mean velocity of the field.
    [Show full text]
  • The Caldwell Catalogue+Photos
    The Caldwell Catalogue was compiled in 1995 by Sir Patrick Moore. He has said he started it for fun because he had some spare time after finishing writing up his latest observations of Mars. He looked at some nebulae, including the ones Charles Messier had not listed in his catalogue. Messier was only interested in listing those objects which he thought could be confused for the comets, he also only listed objects viewable from where he observed from in the Northern hemisphere. Moore's catalogue extends into the Southern hemisphere. Having completed it in a few hours, he sent it off to the Sky & Telescope magazine thinking it would amuse them. They published it in December 1995. Since then, the list has grown in popularity and use throughout the amateur astronomy community. Obviously Moore couldn't use 'M' as a prefix for the objects, so seeing as his surname is actually Caldwell-Moore he used C, and thus also known as the Caldwell catalogue. http://www.12dstring.me.uk/caldwelllistform.php Caldwell NGC Type Distance Apparent Picture Number Number Magnitude C1 NGC 188 Open Cluster 4.8 kly +8.1 C2 NGC 40 Planetary Nebula 3.5 kly +11.4 C3 NGC 4236 Galaxy 7000 kly +9.7 C4 NGC 7023 Open Cluster 1.4 kly +7.0 C5 NGC 0 Galaxy 13000 kly +9.2 C6 NGC 6543 Planetary Nebula 3 kly +8.1 C7 NGC 2403 Galaxy 14000 kly +8.4 C8 NGC 559 Open Cluster 3.7 kly +9.5 C9 NGC 0 Nebula 2.8 kly +0.0 C10 NGC 663 Open Cluster 7.2 kly +7.1 C11 NGC 7635 Nebula 7.1 kly +11.0 C12 NGC 6946 Galaxy 18000 kly +8.9 C13 NGC 457 Open Cluster 9 kly +6.4 C14 NGC 869 Open Cluster
    [Show full text]
  • WIYN Open Cluster Study. XVII. Astrometry and Membership to V
    WIYN Open Cluster Study. XVII. Astrometry and Membership to V = 21 in NGC 188. Imants Platais The Johns Hopkins University, Department of Physics and Astronomy, 3400 N. Charles Baltimore, MD 21218 [email protected] Vera Kozhurina-Platais Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 Robert D. Mathieu Astronomy Department, University of Wisconsin-Madison, 475 North Charter Street, Madison, WI 53706 Terrence M. Girard, William F. van Altena Astronomy Department, Yale University, P.O. Box 208101, New Haven, CT 06520-8101 ABSTRACT We present techniques for obtaining precision astrometry using old photographic plates from assorted large-aperture reflectors in combination with recent CCD Mosaic Imager frames. At the core of this approach is a transformation of plate/CCD coordi- nates into a previously constructed astrometric reference frame around the open cluster NGC 188. This allows us to calibrate independently the Optical Field Angle Distortion for all telescopes and field correctors used in this study. Particular attention is paid to computing the differential color refraction, which has a marked effect in the case of arXiv:astro-ph/0309749v1 27 Sep 2003 NGC 188 due to the large zenith distances at which this cluster has been observed. Our primary result is a new catalog of proper motions and positions for 7812 objects down to V = 21 in the 0.75 deg2 area around NGC 188. The precision for well-measured stars is 0.15 mas yr−1 for proper motions and 2 mas for positions on the system of the Tycho-2 catalog. In total, 1490 stars have proper-motion membership probabilities Pµ ≥ 10%.
    [Show full text]
  • WIYN Open Cluster Study. II. UBVRI CCD Photometry of the Open Cluster NGC 188
    Publications 12-1999 WIYN Open Cluster Study. II. UBVRI CCD Photometry of the Open Cluster NGC 188 Ata Sarajedini Wesleyan University Ted von Hippel Embry-Riddle Aeronautical University, [email protected] Vera Kozhurina-Platais Yale University, [email protected] Pierre Demarque Yale University, [email protected] Follow this and additional works at: https://commons.erau.edu/publication Part of the Stars, Interstellar Medium and the Galaxy Commons Scholarly Commons Citation Sarajedini, A., von Hippel, T., Kozhurina-Platais, V., & Demarque, P. (1999). WIYN Open Cluster Study. II. UBVRI CCD Photometry of the Open Cluster NGC 188. The Astronomical Journal, 188(6). Retrieved from https://commons.erau.edu/publication/226 This Article is brought to you for free and open access by Scholarly Commons. It has been accepted for inclusion in Publications by an authorized administrator of Scholarly Commons. For more information, please contact [email protected]. THE ASTRONOMICAL JOURNAL, 118:2894È2907, 1999 December ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. WIYN OPEN CLUSTER STUDY. II. UBV RI CCD PHOTOMETRY OF THE OPEN CLUSTER NGC 188 ATA SARAJEDINI Department of Astronomy, Wesleyan University, Middletown, CT 06457; ata=astro.wesleyan.edu TED VON HIPPEL Gemini Observatory, 670 AÏohoku Place, Hilo, HI 96720; ted=gemini.edu VERA KOZHURINA-PLATAIS Department of Astronomy, Yale University, New Haven, CT 06520; vera=astro.yale.edu AND PIERRE DEMARQUE Department of Astronomy, Yale University, New Haven, CT 06520; demarque=astro.yale.edu Received 1999 July 21; accepted 1999 August 17 ABSTRACT We present high-precision UBV RI CCD photometry of the old open cluster NGC 188.
    [Show full text]
  • UOCS. V. UV Study of the Old Open Cluster NGC 188 Using Astrosat
    Revised Manuscript J. Astrophys. Astr. (0000) 000: #### DOI UOCS. V. UV study of the old open cluster NGC 188 using AstroSat Sharmila Rani1,2,*, Annapurni Subramaniam1, Sindhu Pandey3, Snehalata Sahu1, Chayan Mondal1, Gajendra Pandey1 1Indian Institute of Astrophysics, Koramangala II Block, Bengaluru, 560034, India 2Pondicherry University, R.V. Nagar, Kalapet, 605014, Puducherry, India 3 Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital, 263001, India *Corresponding author. E-mail: [email protected] MS received XXX; accepted YYY Abstract. We present the UV photometry of the old open cluster NGC188 obtained using images acquired with Ultraviolet Imaging telescope (UVIT) on board the ASTROSAT satellite, in two far-UV (FUV) and one near-UV (NUV) filters. UVIT data is utilised in combination with optical photometric data to construct the optical and UV colour-magnitude diagrams (CMDs). In the FUV images, we detect only hot and bright blue straggler stars (BSSs), one hot subdwarf, and one white dwarf (WD) candidate. In the NUV images, we detect members up to a faintness limit of ∼ 22 mag including 21 BSSs, 2 yellow straggler stars (YSSs), and one WD candidate. This study presents the first NUV-optical CMDs, and are overlaid with updated BaSTI-IAC isochrones and WD cooling sequence, which are found to fit well to the observed CMDs. We use spectral energy distribution (SED) fitting to estimate the effective temperatures, radii, and luminosities of the UV-bright stars. We find the cluster to have an HB population with three stars (T4 5 5 = 4750k - 21000K). We also detect two yellow straggler stars, with one of them with UV excess connected to its binarity and X-ray emission.
    [Show full text]
  • Number of Objects by Type in the Caldwell Catalogue
    Caldwell catalogue Page 1 of 16 Number of objects by type in the Caldwell catalogue Dark nebulae 1 Nebulae 9 Planetary Nebulae 13 Galaxy 35 Open Clusters 25 Supernova remnant 2 Globular clusters 18 Open Clusters and Nebulae 6 Total 109 Caldwell objects Key Star cluster Nebula Galaxy Caldwell Distance Apparent NGC number Common name Image Object type Constellation number LY*103 magnitude C22 NGC 7662 Blue Snowball Planetary Nebula 3.2 Andromeda 9 C23 NGC 891 Galaxy 31,000 Andromeda 10 C28 NGC 752 Open Cluster 1.2 Andromeda 5.7 C107 NGC 6101 Globular Cluster 49.9 Apus 9.3 Page 2 of 16 Caldwell Distance Apparent NGC number Common name Image Object type Constellation number LY*103 magnitude C55 NGC 7009 Saturn Nebula Planetary Nebula 1.4 Aquarius 8 C63 NGC 7293 Helix Nebula Planetary Nebula 0.522 Aquarius 7.3 C81 NGC 6352 Globular Cluster 18.6 Ara 8.2 C82 NGC 6193 Open Cluster 4.3 Ara 5.2 C86 NGC 6397 Globular Cluster 7.5 Ara 5.7 Flaming Star C31 IC 405 Nebula 1.6 Auriga - Nebula C45 NGC 5248 Galaxy 74,000 Boötes 10.2 Page 3 of 16 Caldwell Distance Apparent NGC number Common name Image Object type Constellation number LY*103 magnitude C5 IC 342 Galaxy 13,000 Camelopardalis 9 C7 NGC 2403 Galaxy 14,000 Camelopardalis 8.4 C48 NGC 2775 Galaxy 55,000 Cancer 10.3 C21 NGC 4449 Galaxy 10,000 Canes Venatici 9.4 C26 NGC 4244 Galaxy 10,000 Canes Venatici 10.2 C29 NGC 5005 Galaxy 69,000 Canes Venatici 9.8 C32 NGC 4631 Whale Galaxy Galaxy 22,000 Canes Venatici 9.3 Page 4 of 16 Caldwell Distance Apparent NGC number Common name Image Object type Constellation
    [Show full text]
  • A Catalogue of Star Clusters Shown on the Franklin-Adams Chart Plates” by P.J
    A Catalogue of Star Clusters shown on the Franklin-Adams Chart Plates” by P.J. Melotte – 1915 Mel. # Alternative(s) Type Const. R.A. Dec. Mag. Size Melotte's comments 1 NGC 104 Globular Tucana 00h24m04s -72°05' 4.00 50' A typical globular cluster. Bright. Well condensed at centre. 2 NGC 188, Collinder 6 Open Cepheus 00h47m28s +85°15' 9.30 17' "A somewhat ill-defined cluster mostly 14th to 16th magnitude stars. 3 NGC 288 Globular Sculptor 00h52m45s -26°35' 8.10 13' Globular cluster, rather loose at centre. 4 NGC 362 Globular Tucana 01h03m14s -70°50' 6.80 14' Globular cluster. Similar to N.G.C. 104 but smaller. Bright. 5 NGC 371 Diffuse Nebula Tucana 01h03m30s -72°03' 13.80 7.5' Globular cluster. Falls in smaller Magellanic cloud, and has every appearance of being a globular cluster. A few stars clustering together. Resembles N.G.C. 582, 645, 659. Difficult to decide whether these should not be 6 NGC 436, Collinder 11 Open Cassiopeia 01h15m58s +58°48' 9.30 5.0' classed II. All the clusters here resemble one another though differing in extent. 7 NGC 457, Collinder 12 Open Cassiopeia 01h19m35s +58°17' 5.10 20' A small cluster in a rich region. 8 M103, NGC 581, Collinder 14 Open Cassiopeia 01h33m23s +60°39' 6.90 5' M. 103. A few stars forming a loose cluster. 9 NGC 654, Collinder 18 Open Cassiopeia 01h44m00s +61°53' 8.20 5' A few stars clustered together in a rich region. 10 NGC 659, Collinder 19 Open Cassiopeia 01h44m24s +60°40' 7.20 5' A few stars clustered together.
    [Show full text]