ground based photometry

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S.O. Kepler Brazil

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Ground Based Photometry. S.O. Kepler Brazil. Photometry. Single Channel Two channel: star + comparison Three channel: star+comparison+sky CCD: star + comparisons + skies g-modes in Earth’s atmosphere diffraction rings. CCD. Flat field SNR=1000 : 100 flats at 1% linearity - PowerPoint PPT Presentation

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Page 1: Ground Based Photometry

S.O. KeplerBrazil

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PhotometrySingle ChannelTwo channel: star + comparisonThree channel: star+comparison+skyCCD: star + comparisons + skiesg-modes in Earth’s atmospherediffraction rings

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CCDFlat field SNR=1000 : 100 flats at 1%

linearityAt least 2 comparisons stars, brightAutoguideFrame transfer or low duty cycle or

windowingPrecise timingsQuantum efficiency and altitude variation

affect Amp.

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SX Phe, Rodriguez et al.

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Data reductionTimings for barycenter of the solar systemLeap second correctionsExtinction correctionOptimum extraction: aperture vs seeing

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Multiperiodic

Herbig Ae star, Bernabel et al.

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Fourier TransformsNoise not poissonicData not equally spacedNeed Monte Carlo simulation for false alarm probabilityIdentification of multiple modes: pre-whitening

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2.1m4.1m

Frequency

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Low amplitude pulsators

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DistanceParallax 95 + 37 pcOptical Spectra 58 + 02 pcIUE flux 59 + 05 pcHST flux 67 + 04 pcSeismology Bradley 1998 61pcSeismology Benvenutto et al. 2002 63 pcMean: 67 + 14 pc

215s

270s304s

107s119s

125s

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PG1336-018,Maia Vuckovic

Vik Dhillon, Stuart Littlefair, and Paul Kerry (Sheffield, UK), Tom Marsh (Warwick, UK), Andy Vick and Dave Atkinson (UKATC, Edinburgh, UK)

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STEPHI Date Object # freq Noise level Effective duration PI I 06/87 63 Her 6 . . J.A. Belmonte II 08/89 GX Peg 5 1.5 E-4 219h E. Michel III 11/90 V650 Tau 4 7.6E-4 167h E. Michel IV 02/92 BUCnc 6 7.6E-4 (3.E-4) 228h J.A. belmonte . // BNCnc 5 7.6E-4 (2.E-4) // // V 09/93 VW Ari 7 6.E-4 150h Liu Y.Y. VI 02/95 BQ Cnc 9 4.E-4 (1.7E-4) 210h M. Alvarez . // BWCnc 3 // // // VII 02/96 BS Cnc 3 7.7E-4 115h M. Hernandez . // BT Cnc 2 // // // VIII 11/97 V647 Tau 5 1.6E-4 228h E. Michel IX 11/98 V534 Tau 11 2.5E-4 286h Li Z.P. X 12/99 V624 Tau 7 3.0E-4 269h L. Fox Machado . // HD23194 2 4.2E-4 // // XI 11/02 HD23628 . . . J. Peña . // HD23567 . . . // XII 06/03 7 Aql . . . L. Fox Machado 8 Aql // XIII 06/04 HD172189 E. Michel XIV 11/05 in progress XV 10/06 in progress

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DSN CampaignsDSN 1 Theta 2 Tauri 1983 DSN 2 4 CVn 1984 DSN 3 Theta 2 Tauri 1986 DSN 4 HR729 1988 DSN 5 BU Cnc & EP Cnc 1989 DSN 6 63 Her 1990 DSN 7 HN CMa 1990 DSN 8 CD -24 7599 1992 DSN 9 FG Vir 1993 DSN 10 IC 418 1993 DSN 11 CD -24 7599 1994 DSN 12 Theta 2 Tauri 1994 DSN 13 IC 418 1994 DSN 14 FG Vir 1995 DSN 15 4 CVn 1996

DSN 16 4 CVn 1997 DSN 17 CD -24 7599 1998 DSN 18 BI CMi 1998/1999 DSN 19 BI CMi 1999/2000 DSN 20 44 Tau 2000 DSN 21 44 Tau 2001

DSN 22 FG Vir 2002

DSN 23 FG Vir 2003 DSN 24 44 Tau 2003

DSN 25 FG Vir 2004, 79 freqs

DSN 26 44 Tau 2004 DSN 27 HD210111 & ,AS Eri

2005 DSN 28 UV Oct & SS For 2005 DSN 29 44 Tau 2005

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Whole Earth Telescope XCov1 Mar 1988 *PG 1346+082* IBWD Winget, Provencal V803 Cen IBWD O'Donoghue XCov 2 Nov 1988 *G29-38* DAV Winget V471 Tau ICBS Clemens XCov 3 Mar 1989 *PG 1159-035* GW Vir Winget XCov 4 Mar 1990 *AM CVn* IBWD Solheim, Provencal G117-B15A DAV Kepler XCov 5 May 1990 *GD358* DBV Winget GD165 DAV Bergeron HD 166473 roAp Kurtz XCov 6 May 1991 *PG 1707* GW Vir Clemens, Pfeiffer GD154 DAV Vauclair XCov 7 Feb 1992 *1H0857* CV Buckley PG 1115 DBV Barstow, Clemens G226-29 DAV Kepler WET-0856 d Scu Breger, Handler XCov 8 Sep 1992 *PG 2131+066* GW Vir Kawaler, Nather G185-32 DAV Moskalik RX J2117 GW Vir Vauclar, Moskalik XCov 9 Mar 1993 *PG 1159-035* GW Vir Winget *FG Vir* d Scu Breger XCov 10 May 1994 *GD358* DBV Nather, Bradley XCov 11 Aug 1994 *RX J2117* GW Vir Vauclar, Moskalik XCov 12 Apr 1995 *PG 1351* DBV Hansen L19-2 DAV Sullivan, Clemens XCov 13 Feb 1996 *RE 0751+14* CV Marar, Seetha CD-24 7599 d Scu Breger, Handler XCov 14 Sep 1996 *PG 0122+200* GW Vir O'Brien WZ Sge CV Nather XCov 15 Jul 1997 *DQ Her* CV Nather EC 20058 DBV O'Donoghue

XCov 16 May 1998 *BPM 37093* DAV Kanaan, Kepler XCov 17 Apr 1999 *PG 1336* sdB Kilkenny *BPM 37093* DAV Kanaan, Kepler, Nitta,

Winget XCov 18 Nov 1999 *HL Tau 76* ZZ Ceti Dolez, Vauclair,

Kleinman PG 0122 DOV Vauclair, O'Brein XCov 19 June 2000 *GD358* DBV Kepler, Nitta XCov 20 Nov 2000 *HR 1217* roAp Kurtz KUV 05134+2605 DBV Handler, Nitta R 548 ZZ Ceti Mukadam XCov 21 Apr 2001 *PG 1336* sdb Reed, Kilkenny PG 1654-160 DBV Handler Feige 48 sdB Reed, Kawaler Mrk 501 AGN Miller, Krennrich Xcov 22 May 2002 *PG 1456+103* DBV Handler PG 1159-035 GW Vir O'Brein Feige 48 sdB Reed, Kawaler PG 1605+072 sdB Schuh, et. al, & MSST XCov 23 Aug 2003 *KPD 1930+2752* sdB Charpinet,

Reed G 29-38 DAV Kleinman HS 2201+2610 sdB Silvotti XCov 24 Oct 2004 *PG 0014* sdB Kawaler RX J2117 GW Vir Moskalik XCov 25 Jul 2006 GD358 DBV Provencal XCOV 26 Mar 2008 EC14012-114 DAV Montgomery PG1159-035 DOV Costa

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Don KurtzMargarida Cunha

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k=14 - 42

J. Edu S. Costa

PG1159-035

-no harmonics or combination modes-no convection zone- 198 modes: 29 triplets, 46 quintuplets

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Period(s)

PG1159-035

P=21.43+0.05sM=0.586+0.001MSun

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Córsico et al. 2008

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dP/dt=(+10.6+0.1)x10-11 s/s

E(cycles)

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Costa & Kepler 2008: rotation, contraction rates, cooling ratesdP/dtdPRotation/dtdR/dtdT/dt

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Rotation effectsMultiplets have different amplitudes Amplitudes change (energy exchange with

rotation?)Gough: “Only when the star is rotating is

there a physically real principal axis …with a well defined directed orientation … So if there is an m = +1 , m = −1 asymmetry … it has to be a consequence of rotation.”

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ZZ Ceti white dwarf

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Mike Montgomery

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Hydrogen layer mass

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Questions on mode properties What are the driving, mode selection, and amplitude limiting

mechanism(s)? Are they the same for all strips and throughout each strip? What is the cause of the amplitude and phase changes on

timescales from weeks to years? What is the origin, role, and nature of mode coupling? What is the role of inclination in m-selection, considering we see the

amplitude of different m components change with time in a few stars? Can we measure the velocity and line profile variations needed for

mode identification, necessary for full asteroseismic analysis? Are there other values of the spherical harmonic degree, besides 1

and 2 already observed in white dwarfs? High l have been identified in sd.

Is driving different for different pulse shapes, or for the DOVs, where the models do not indicate significant convection?

Can we identify the modes with chromatic amplitude and combination peaks?

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