RR Lyrae Stars for SIM I. Making the B-List II. Obtaining Apparent Mags: (a) Field and (b) Cluster.

Slides:

Advertisements

Similar presentations

Variable Stars of Globular Clusters in the Large Magellanic Cloud Evan McClellan (FSU) Horace Smith (advisor) (MSU) Charles Kuehn (MSU) August 6 th, 2008.

Advertisements

An Abundance Spread in the Bootes I Dwarf Spheroidal Galaxy? John E. Norris The Australian National University Gerard Gilmore University of Cambridge R.F.G.

A new flare star member candidate in the Pleiades Cluster (Moualla et al.) This Study Initially undertaken to find new low-mass stars, brown dwarfs and.

Astronomy C - Variable Stars A. Pulsating Variables: 1) Long Period Variables a) Mira type b) Semiregular 2) Cepheids 3) RR Lyrae 4) RV Tarui B. Cataclysmic.

Collaborators:  K. Krisciunas (CTIO/Carnegie), N. Suntzeff (CTIO)  M. Hamuy (Carnegie), E. Persson (Carnegie), W. Freedman (Carnegie), M. Roth (Carnegie)

Intense observations of RR Lyr stars Dr. F.-J. (Josch) Hambsch VVS, GEOS, BAV, AAVSO.

ECLIPSING BINARIES IN OPEN CLUSTERS John Southworth Dr Pierre Maxted Dr Barry Smalley Astrophysics Group Keele University.

Thanks to Henrietta Swan Leavitt, Harvard CfA November 5th Hommage to Henrietta Leavitt from the CoRoT Team Annie BAGLIN, Merième CHADID,

Variable Stars in the Globular Cluster NGC 6496 Katherine Guldenschuh & Andrew Layden (Bowling Green State University) Douglas Welch (McMaster University),

Variable Stars:Pulsation, Evolution and applications to cosmology Shashi M. Kanbur SUNY Oswego June 2007.

RR Lyrae Stars as a Tool to Measure Interstellar Reddening Andrew Layden, Brad Boswell, et al. Bowling Green State University Variable Stars 2004, BGSU,

Basic Astrometric Methods William van Altena Yale University Basic Astrometric Methods Yale University July 18-22, 2005.

RR Lyrae Observations M B,V,I,K = m B,V,I,K - 5 log d + 5 To calibrate M B,V,I,K we need: To calibrate M B,V,I,K we need: BVIK light curves for field RRL.

ECLIPSING BINARIES IN OPEN CLUSTERS John Southworth Jens Viggo Clausen Niels Bohr Institute Københavns Universitet.

Fourier Analysis Fourier analysis is an important part to analyzing scientific data from RRab light curves. It is a mathematical process by which a curve.

Omega Centauri, Cambridge The RR Lyrae of  Centauri: a theoretical route The RR Lyrae of  Centauri: a theoretical route (progress report) Castellani.

Variable Stars in NGC 6304 Nathan De Lee (MSU) Horace Smith (Advisor) (MSU) Barton Pritzl (Macalester College) Marcio Catelan (PUC) Allen Sweigart (GSFC)

WOCS Variability: Monitoring NGC6939 S. Kafka (IUB) D. Gibbs II (Univ. of Wyoming) A. Henden (US Naval Obs.) R.K.Honeycutt (IUB) S. Kafka (IUB) D. Gibbs.

Chemically Peculiar/Magnetic Stars and the  a photometry Hans Michael Maitzen, Ernst Paunzen Institute for Astronomy, University of Vienna.

1 RR Lyrae Stars for SIM I. A- and B-Lists II. Obtaining Apparent Mags: (a) Field and (b) Cluster.

X-ray Optical microwave Cosmology at KIPAC. The Survey 5000 square degrees (overlap with SPT and VISTA) Five-band (grizY) + VISTA (JHK) photometry to.

Seattle University and APO Joanne Hughes Department of Physics.

Variable Stars in the Old Dwarf Spheroidal Galaxies, SDSS dSph’s, and Globular Clusters Charles Kuehn Michigan State University.

Photometry and Astrometry of SIM Planetquest Globular Cluster Targets T. M. Girard (Yale), A. Sarajedini (U. Florida), B. Chaboyer (Dartmouth) Table 1.

The Chinese SONG proposal: scientific concerns Jianning Fu (Beijing Normal University) and Chinese SONG team Beijing ─ March 29, 2010 The third workshop.

IAS, June 2008 Caty Pilachowski. Visible in the Southern Sky Listed in Ptolemy's catalog Discovered by Edmond Halley in 1677 –non-stellar –"luminous spot.

1 AGB variables; Distance Indicators; Bolometric Magnitudes; Pulsation Modes. Michael Feast University of Cape Town and South African Astronomical Observatory.

RR Lyraes Bi-Qing For Chris Sneden (UT) George Preston (Carnegie Observatory)

New and Odds on Globular Cluster Stellar Populations: an Observational Point of View (The Snapshot Database) G.Piotto, I. King, S. Djorgovski and G. Bono,

25 Years of Globular Clusters with HST

H-R diagrams for star clusters. H-R Diagram Relation between luminosity L, temperature T and radius R: L = 4  R 2  T 4.

Star Clusters. Pre clusters Courtesy University of Oregon.

Light Elements (Li and Be) in Globular Clusters L. Pasquini, ESO  Li in Turn-Off (or close to TO)  Li in evolved stars  A new result..  Be in TO stars.

Star Groups Chapter 27 (p ). Galaxies Def: large groups of stars (approx. 100 billion) bound by gravitational attraction Also contain gas and.

ASTR112 The Galaxy Lecture 4 Prof. John Hearnshaw 7. Globular clusters 8. Galactic rotation 8.1 From halo stars 8.2 From disk stars – Oort’s constant,

Variable Stars & Distance The “Standard Candle”.

EXPLORE/OC: Photometry Results for the Open Cluster NGC 2660 K. von Braun (Carnegie/DTM), B. L. Lee (Toronto), S. Seager (Carnegie/DTM), H. K. C. Yee (Toronto),

Image Stability  ACS SMOV image stability test (prop 9017) went from a cold soak (anti-solar pointing) for 8 orbits to a hot attitude (including off-nominal.

RR Lyrae Stars By: Mike Lundquist.

Parallax Luminosity and mass functions - a few basic facts Kinematics of the solar neighborhood Asymmetric drift Thin disk, thick disk Open and globular.

基督再來（一）. 經文： 1 你們心裡不要憂愁；你們信神，也當信我。 2 在我父的家裡有許多住處；若是沒有，我就早已告訴你們了。我去原是為你們預備地去。 3 我若去為你們預備了地方，就必再來接你們到我那裡去，我在那裡，叫你們也在那裡， ] ( 約 14 ： 1-3)

How do we use RR Lyrae to measure distances? RS Boötis Rachel Zheng UC Davis COSMOS Cluster 4 Astrophysics 2015.

An Abundance Spread in the Bootes I Dwarf Spheroidal Galaxy? John E. Norris The Australian National University Gerard Gilmore University of Cambridge R.F.G.

BIS 219 Complete Class Check this A+ tutorial guideline at Complete-Class. For more classes visit

BIS 219 Week 2 DQ 2 What are some of the issues inherent in managing data? What methods may be used to identify data management issues? As a manager, how.

BIS 220 Week 2 Individual Information Systems Proposal Check this A+ tutorial guideline at 220/BIS-220-Week-2-Individual-Information-

BIS 220 Week 4 Learning Team Wireless Technologies Proposal Check this A+ tutorial guideline at 220/BIS-220-Week-4-Learning-Team-

BIS 303 Complete Class Check this A+ tutorial guideline at S-303/BIS-303-Complete-Class-Guide For more classes visit.

BIS 318 Complete Class Check this A+ tutorial guideline at Complete-Class-Guide For more classes visit.

BIS 320 Complete Class Check this A+ tutorial guideline at 320/BIS-320-Complete-Class-Guide For more classes visit.

Near-IR Diagnostics for SNe Carnegie Observatories

Identification of RR Lyrae Stars in the Milky Way Nuclear Star Cluster

Globular Cluster Astrometry

RR Lyrae variable stars

Godrej Prakriti Sodepur | Godrej Prakriti Kolkata

Peculiar Massive Globular Clusters in the Milky Way

RR Lyrae Research with the Kepler Mission

Giftalove Best Cake Offers

Master thesis Detection of Van Hoof effect in RR Lyrae stars from BOES observation Spectroscopy for RR Lyrae variables Target : TT Lyn, RR Leo, & SW Dra.

The “Milky Way”.

Слайд-дәріс Қарағанды мемлекеттік техникалық университеті

.. -"""--..J '. / /I/I =---=-- -, _ --, _ = :;:.

II //II // \ Others Q.

I1I1 a 1·1,.,.,,I.,,I · I 1··n I J,-·

Lab 9 – Ages and Distances to Clusters

Variable Stars.

. '. '. I;.,, - - "!' - -·-·,Ii '.....,,......, -,

Presentation transcript:

RR Lyrae Stars for SIM I. Making the B-List II. Obtaining Apparent Mags: (a) Field and (b) Cluster

B-List 5-10 more RRc 5-10 more RRc All RRab with: All RRab with: [Fe/H] > -1.0 [Fe/H] > -1.0 [Fe/H] < -2.0 [Fe/H] < -2.0 (~8 stars) (~8 stars) More at disk/halo: More at disk/halo: [Fe/H] ~ -1 [Fe/H] ~ -1 (~5 stars) (~5 stars) More at OoI/II: More at OoI/II: [Fe/H] > -1.5 [Fe/H] > -1.5 (20+ stars?) (20+ stars?) Will prioritize (40-84) Will prioritize (40-84)

BVIK light curves of Field RRL 60 field RRL in A-List 60 field RRL in A-List BVI: BVI: Most have PE/CCD B,V light curves Most have PE/CCD B,V light curves Have been obtaining I with BGSU 0.5m+CCD Have been obtaining I with BGSU 0.5m+CCD Plan to do all stars w/  > -20° by Dec 2004 Plan to do all stars w/  > -20° by Dec 2004 K: K: 16 stars need K, most in South 16 stars need K, most in South Have queue-scheduled 1.3-m O/IR at CTIO Have queue-scheduled 1.3-m O/IR at CTIO

BGSU 0.5m+CCD

Locations of 60 Field RRL

BVIK LCs of Cluster RRL K: K: Will need to do most clusters: ~15 visits each Will need to do most clusters: ~15 visits each Begin in 2005? (SOAR, LCO, MDM?) Begin in 2005? (SOAR, LCO, MDM?) BVI: BVI: 6 of the 13 RRL-bearing globulars have BVI 6 of the 13 RRL-bearing globulars have BVI 4 need BVI: M13, M30, NGC362, NGC need BVI: M13, M30, NGC362, NGC6723  Cen needs BI  Cen needs BI M55 and 47 Tuc need I M55 and 47 Tuc need I

BVI data on RRL in Globulars Obtained w/ CTIO 0.9-m & LCO 40”: Obtained w/ CTIO 0.9-m & LCO 40”:  Cen: 66 visits in BI … done!  Cen: 66 visits in BI … done! NGC 362: 25 visits in BVI … done? NGC 362: 25 visits in BVI … done? 47 Tuc: 20 visits in I … done? 47 Tuc: 20 visits in I … done? NGC 6732: 7 visits in BVI … needs more NGC 6732: 7 visits in BVI … needs more Time on CTIO 0.9-m to continue in Feb ‘04 Time on CTIO 0.9-m to continue in Feb ‘04 Will do photometry in Summer 2004 Will do photometry in Summer 2004 Propose to CTIO 0.9-m to do M30 & M55? Propose to CTIO 0.9-m to do M30 & M55? Propose to WIYN 0.9-m to do M13?? Propose to WIYN 0.9-m to do M13??