Andrzej Pigulski

astro.phys.au.dk

Andrzej Pigulski

Variability survey in Kepler fieldwith ASAS-NorthobservationsA. PigulskiAstronomical Institute, Wrocław UniversityG. Pojmański,D.Szczygieł, B.PileckiWarsaw University ObservatorySecond KASC workshop, Aarhus, June 10, 2008


GCVS = General Catalogue of Variable StarsAll: 185● with 9 m < V < 15 m : 117○ brighter than 9 m : 26 or fainter than 15 m : 42


NSV = New Suspected VariableAll: 100● with 9 m < V < 15 m : 52○ brighter than 9 m : 26 or fainter than 15 m : 22


ROTSE1 catalog (Akerlof et al. 2000)All: 148● with 9 m < V < 15 m : 148


NSVS ROTSE1 red catalog variables (Akerlof (Williams et al. et 2000) al. 2004)All: 115 148● with 9 m < V < 15 m : 148 115


HATnet (Hartman et al. 2004)All: 239● with 9 m < V < 15 m : 239


Observations:June-July 2003HATnet #199 field (Hartman et al. 2004) 8.3º x 8.3º


GCVS+NSV+ROTSE1+NSVSred+HATHATnet (Hartman et al. 2004)All: 239 633● with 9 m < V < 15 m : 239 521○ brighter than 9 m : 52 or fainter than 15 m : 60


VARIABLES in OPEN CLUSTERSNGC 6866log(age) = 8.6Var: a fewWrocław search (unpub.)NGC 6811log(age) = 8.8Var: ~15Van Cauteren et al. (2005)Wrocław search (unpub.)NGC 6819log(age) = 9.2Var: ~190 (faint)Street et al. (2002, 2005)NGC 6791log(age) = 9.6Var: ~330 (faint)Mochejska et al. (2003, 2005)de Marchi et al. (2007)


All Sky Automated Survey (ASAS)Site: Las Campanas ObservatoryP.I.:.: Grzegorz Pojmański,Warsaw ObservatoryCo.I: Danuta Szczygieł, , Bogumił Pilecki, Warsaw ObservatoryRange in V: 7 – 14 mag (observations(both in V and I)ASAS-1: : 1997: Test observationsASAS-2: : 1997 - 2000, 300 sq. deg. . (0.7%(of the sky), 140 000 stars.3900 variable stars found.ASAS-3: : 2000 - now 70 % of the sky !!! (δ < +28º), 15 × 10 6 stars.50 000 variable stars.ASAS-NorthNorth: : 2006 - now (site: Mauna Kea)


ASAS-NorthSix ASAS fields covering Kepler FoV were selected.The fields contain 9.1 × 10 5 stars of which about 27%(i.e. 248 700) fall within Kepler FoV.V and I photometry is available.~90 V-filter and ~110 I-filter data points on average.The observed range in V (7-15 mag) matchesvery well that of Kepler


ASAS-North: distribution in timeVsampleV-filter dataHJD 2450000.+Amplitude [mag]Frequency [d -1 ]


ASAS-North: distribution in timeIsampleI-filter dataHJD 2450000.+Amplitude [mag]Frequency [d -1 ]


ASAS-North: detection threshold


ASAS-NorthAll: 887 + 175 suspects● with 9 m < V < 15 m : 818○ brighter than 9 m : 46 or fainter than 15 m : 23


ASAS-North● already known: 268● new: 619


MirasAll: 71● with 9 m < V < 15 m : 66○ brighter than 9 m : 2 or fainter than 15 m : 3


ROTSE1 J193032.71+480327.0V2285 CygASAS 193033+4803.4VI


Long-period variables (LB, SR)All: 642● with 9 m < V < 15 m : 598○ brighter than 9 m : 24 or fainter than 15 m : 20


ASAS 192433+5014.5 = CH Cyg(symbiotic star)VI


CepheidsASAS 192345+5116.2(P = 13.375 d)ASAS 192152+4911.9(P = 3.458 d)ASAS 194815+4307.6 = V1154 Cyg(P = 4.926 d)ROTSE1 J191853.61+434930.0 =ASAS 191854+4349.5 = V2279 Cyg(P = 4.133 d)V1673 Cyg(RV Tau?)All: 5● with 9 m < V < 15 m : 5


V1154 CygVV2279 CygASAS 192345+5116.2ASAS 192152+4911.9I


ASAS 192345+5116.2P = 3.458 dVI∆V ≈ 0.4 mag∆I ≈ 0.25 mag


ASAS 192152+4911.9P = 13.375 dVI∆V ≈ 0.4 mag∆I ≈ 0.4 mag


Eclipsing binariesAll: 301● with 9 m < V < 15 m : 272○ brighter than 9 m : 4 or fainter than 15 m : 25


RR Lyrae starsAll: 49 (41 RRab + 8 RRc)● with 9 m < V < 15 m : 28○ brighter than 9 m : 1 (RR Lyr) or fainter than 15 m : 20


RRab: ASAS 192325+4231.7 (P = 0.6836 d)VRRc: ASAS 190350+4601.7 = ROTSE1 J190350.47+460144.8 (P = 0.3659 d)I


Other pulsators(β Cep, δ Sct, γ Dor, SPB)● P < 0.1 d: 168● 0.1 d < P < 0.3 d: 57● 0.3 d < P < 5 d: 65● P > 5 d: 21


High-amplitude δ Scuti Star (HADS)ASAS 190816+4957.3P = 0.06118 dVI


β Cephei stars?V543 Lyr (B3 V) : candidate acc. to Stankov & Handler (2005),frequency of 10.72 d-1 fro Hipparcos(Koen & Eyer 2002)V819 Cyg (B0.5 IIIn): P = 0.71373 d (Koen & Eyer 2002)V558 Lyr (B3 Ve): P = 0.60972 & 0.62625 (Molenda-Żakowicz& Połubek V2005)If close to the Galactic plane, should be bright, probablybrighter than the limit of V = 9 mag.Observe all early B-type stars that could be selected ?I

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