전영범 성현일 KASI 한장희 이종택 한국교원대학교 Richard de Grijs Kavli Institute for Astronomy amp Astrophysics Rodolfo Angeloni la Pontificia Universidad CatolicaPUC ID: 795418
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Slide1
The VVV Templates Project
전영범, 성현일 (KASI)한장희, 이종택 (한국교원대학교)Richard de Grijs (Kavli Institute for Astronomy & Astrophysics)Rodolfo Angeloni (la Pontificia Universidad Catolica(PUC) -Chile)
손정주 (한국교원대학교)
2014 Survey Science Group Workshop
Slide2Slide3VVV Project
The Vista Variables in the Vía Láctea (VVV) ESO Public SurveyESO's Visible and Infrared Survey Telescope for Astronomy 4 m telescopea wide near-infrared (IR) camera (VIRCAM)a mosaic of 16 2048x2048 detectors0.8-2.5 micronan average pixel scale of 0.34"/pixelFoV : 1.1x1.5 square degrees1 magnitudes deeper than their 2MASS counterpartsprovide a window into time-variable phenomenaa time span of about 5 years, with a total of 1929 hours of observing time
Slide4VVV Project
Of order 109 point sources within a total sky area of 520 deg2 will be monitored.The surveyed region includes 36 globular clusters and about 314 known open clusters. A deep IR atlas in 5 passbands and a catalogue containing an estimated 106 variable stars.
Slide5Light Curve Templates in the Near-IR: Towards Automated Classification of VVV Light Curves for Cataclysmic Variable Stars
Cataclysmic Variables have been extensively observed at optical, ultraviolet, and X-ray wavelengths, where their white dwarf primary stars and bright accretion disks dominate the spectral energy distribution. Unfortunately, little is known about their infrared properties. The assumption that infrared observations would reveal only the “uninteresting” secondary star has been shown to be false, as recent investigations have instead shown.A shorter time-scale it will provide a unique chance of enlarging our specific knowledge of the cataclysmic phenomenon. In particular, time-series of NIR photometry would allow us to measure the ellipsoidal variations of the tidally distorted mass-donor star as well as irradiation effects. By modeling the modulation, we could then put strong constraints on fundamental parameters such as the geometry of the binary, and, in case of the contribution of the mass-donor star in two or more bands is known, it is possible to infer its spectral type (and surface temperature) and to estimate the distance to the binary via photometric parallax.
Slide6Light Curve Templates in the Near-IR: Towards Automated Classification of VVV Light Curves for Cataclysmic Variable Stars
Unlike previous variability surveys, such as MACHO and OGLE, the VVV Survey will be carried out in the near-IR, mainly in the K band. While this will allow us to probe deeper into the heavily obscured regions of the Galactic bulge and plane than ever before, it also presents us with important challenges. In particular, the extensive, high-quality templates that are needed for automated variable star classification algorithms are not available in the near-IR. We have thus to build a large database of well-defined, high-quality, near-IR light curves for variable stars of different types, which will form the basis for the VVV automated classification. This database will be critical for the successful outcome of the VVV Survey.
Slide7Light Curve Templates in the Near-IR: Towards Automated Classification of VVV Light Curves for Cataclysmic Variable Stars
In order to properly classify as a template, a light curve must meet some minimum observational criteriafirst, the observations must be very precise, with the relative error in the photometry being less than about 1/10 of the light curve amplitude. Second, the light curve itself must be complete, without any clear gaps. This is of great importance to properly compute accurate Fourier decomposition parameters for the light curves, as needed in order to feed the automated classification algorithms.Jones et al. (1996)
Slide8VVV Templates Project
SCIENTIFIC GOALSThe main goal is to derive well-defined light curve templates in the near-IR for the automated classification of VVV light curves.RR Lyrae stars in the globular cluster ω Centauri (Del Principe et al. 2006).
Slide9VVV Templates Project
Targets # Name α (J2000) δ (J2000) K mag. P[d] Var. type--------------------------------------------------------------------------------------------------01) V
Sge 20 20 14.69 +21 06 10.39 9.811 0.5142
Novalike
,
Supersoft
X-ray source
02) AE
Aqr
20 40 09.16 -00 52 15.07 8.780 0.4151 Intermediate Polar
02) UU
Aqr
22 09 05.76 -03 46 17.70 12.483 0.1636 SW Sex star
03) FO
Aqr
22 17 55.38 -08 21 03.90 12.508 0.2018 Intermediate Polar
04) AO
Psc
22 55 17.99 -03 10 40.00 13.088 0.1496 Intermediate Polar
05) IP Peg 23 23 08.55 +18 24 59.30 11.721 0.1582 Dwarf Novae
06) RX And 01 04 35.54 +41 17 57.80 11.56 0.2099 Z Cam star
07) HT
Cas
01 10 13.13 +60 04 35.40 13.84 0.0736 SU
UMa
star
08) AY Psc 01 36 55.45 +07 16 29.30 14.002 0.0993 Nova-like, RW Tri star09) RW Tri 02 25 36.15 +28 05 50.90 11.46 0.2319 Nova-like variable10) GK Per 03 31 11.82 +43 54 16.80 ~13 1.9968 Intermediate Polar, Fast Novae11) V1309 Ori 05 15 41.41 +01 04 40.50 13.512 0.3326 polar/AM Her system12) U Gem 07 55 05.24 +22 00 05.10 10.83 0.1769 SS Cyg star13) SU UMa 08 12 28.26 +62 36 22.50 11.670 0.0076 Prototype of the SU UMa stars14) Z Cam 08 25 13.20 +73 06 39.23 10.856 0.2898 Prototype of the Z Cam stars15) GY Cnc 09 09 50.55 +18 49 47.50 13.118 0.1754 SS Cyg star
Slide10Telescopes
EuropeItaly - Osservatorio Astronomico di Padova (INAF-OAPd) 92cm Telescope, delta Scuti, SX PheSpain - Instituto de Astrofísica de Canarias (IAC) 1.52m, CAIN III, delta Scuti, SX Phe
Slide11Telescopes
AfricaIRSF Telescope : 1.4m, RR Lyrae in globular clusters (M62, NGC1851), delta Scuti in open clusters (NGC6134)0.75-m Telescope : delta Scuti, SX Phe, Ellipsoidal, Eclipsing binaries
Slide12Telescopes
North AmericaCanadaMaxico : 2.12 m, CANICA beta Cephei and delta ScutiSouth AmericaChileAsiaKazakshutanSouth Korea : 1.8 m BOAO
Slide13Bohyunsan
Optical Astronomy Observatory (BOAO)
Slide14KASINICS
(KASI Near Infrared Camera System) - cooling temperature : sensor part = 30K - temperature of cold box < 80K - Pixel scale : 0.39" x 0.39" - Field of view : 3.3' x 3.3' - Gain(e-/ADU) : 2.56 - Readout Noise : 39 electrons - Dark Current : 18.2 electrons/sec - Average Seeing(BOAO) : 1.5" ~ 1.7" - Filter : total 6 (J, H, Ks, L, H2, H3+)
Slide15Light Curve of BL Cam
: The Preliminary result of VVV light curve templates R.A. (J2000) 03h 47m 19.8s Dec. (J2000) +63°22’43” Brightness <V> ~ 13.1mag Period [d/h] 0.03909/0.93834 - Low metallicity ([Fe/H]=-2.4) High amplitude Short period and multi - periodicity One of well known 12 field SX
Phe star
BL Cam, 2MASS
Slide16Light Curve of IP Peg
: The Preliminary result of VVV light curve templatesα(J2000) : 23 23 08.55, δ(J2000) : +18 24 59.30 K mag : 11.721, P[d/h] : 0.1582/3.7968 dwarf nova - U Gem type 동반성에서 백색왜성을 둘러싸고 있는 강착원반으로 물질 유입이 이루어지고 있는 천체.불규칙한 주기의 outburst – 가시광에서 2등급 정도 밝아지는 것으로 알려져 있음.Inclination : 80° ～ 85°Mass ratio (q)=0.42Distance = 115±30 pc to the system
Slide17Name
period(d/h)observation timedataIPPeg
0.1582/3.7968
19:20
–
2:30
8h
관측
(2
주기
)
RW Tri
0.2319/5.5656
20:30
–
5:00
7h
관측
(1.3
주기
)
UU Aqr
0.1636/3.9264
19:20
–
00:20
5h 관측(1.2주)BL Cam0.03909/0.9383420:30 – 5:005h 관측(5주기)V1007Cas 0.0332/7.96819:20 – 4:40
9h
관측
(1.1
주기
)
V2416Cyg
0.05589/1.34136
19:20
–
1:00
7h
관측
(5.3
주기
)
AY Psc
0.0993/2.3832
20:30
–
4:30
KV Per
0.2491/5.9784
19:20
–
5:00
8h
관측
(1.3
주기
)
RX And
0.2099/5.0376
19:20 – 5:002h 관측(0.4주기)V460And0.0749808/1.8 20:00 – 5:009h 관측(5주기)AM Her 0.1289/3.093619:20 – 23:00V1047 Her0.3207/7.69682:30 – 5:0024h 관측(3주기)BO Lyn0.0934 / 2.241619:20-21:0036h 관측(16주기)
Light Curve
of CVs
: The Preliminary result of VVV light curve templates
Slide18Thank you!