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Astro Back to Astronomy MAPPING THE HIDDEN MILKY WAY VVV Survey SOL how did the Milky Way form VISTA PUBLIC SURVEYS ~100 epochs ~109 stars ~10 6 variables 520 sq.deg. VVV FoF Workshop Observatorio Cordoba, Argentina, April 2011 Dante Minniti obtain a 3-D bulge map using RR Lyrae vvvsurvey.org identify variables belonging to known star clusters find high PM BDs discover new open and globular clusters study distant SN map star forming regions along the Galactic plane ...... find eclipsing binaries and detect planetary transits ...... VVV Goals search for microlensing events discover high velocity stars study rare variable sources identify SN light echoes monitor the variability around the Galactic center map spiral arms find variable stars in the Sgr dwarf galaxy census TNOs ... recognize background QSOs Asociacion Argentina de Astronomia La Plata, Sep 2009 Dante Minniti... what is the 3-D structure of the inner MW vvvsurvey.org • 2-D MW maps are not sufficient, need 3-D • a single snapshot is not sufficient, need time coverage 2MASS JHK vvvsurvey.org Bulge 300 sq deg: -10º < l < +10º ; -10º < b < +5º Disk 220 sq deg: -65º < l < -10º ; - 2º < b < +2º 2MASS JHK x% of MW Asociacion Argentina de Astronomia La Plata, Sep 2009 Dante Minniti vvvsurvey.org Expected monthly dataflow: raw calibrations and science frames from Magda Arnaboldi (EDT) VISTA and the VLTs at Paranal VISTA TELESCOPE vvvsurvey.org AT ESO PARANAL 4.1 m telescope f3.25 focus fov 1.5 sqdeg vvvsurvey.org VISTA Near-IR Wide Field Camera 16x 2048x 2048 VIRGO IR detectors large numbers of hot pixels, dead zones in detector 1 sensitivity: 0.84 to 2.5 microns filters: Z, Y, J, H, Ks pixel scale: 0.34¨ active optics “tile” field of view: 1.0x1.5 deg (6 pointings) best image quality: 0.6¨ (incl. seeing, optics, sampling) image distortion: <15% of PSF at field corners vvvsurvey.org VVV Tiles Ignacio Toledo b271 b372 b322 b274 b323 SV b349 d003 d014 vvvsurvey.org VVV Year 1 VVV Survey Area and Tile numbers 396 395 394 393 392 391 390 389 388 387 386 385 384 383 +4 382 381 380 379 378 377 376 375 374 373 372 371 370 369 +2 368 367 366 365 364 363 362 361 360 359 358 357 356 355 354 353 352 351 350 349 348 347 346 345 344 343 342 341 152 151 150 149 148 147 146 145 144 143 142 141 140 139 138 137 136 135 134 133 132 131 130 129 128 127 126 125 124 123 122 121 120 119 118 117 116 115 114 113 112 111 110 109 108 107 106 105 104 103 102 101 100 99 98 97 96 95 94 93 92 91 90 89 88 87 86 85 84 83 82 81 80 79 78 77 +0 340 339 338 337 336 335 334 333 332 331 330 329 328 327 326 325 324 323 322 321 320 319 318 317 316 315 314 313 76 75 74 73 72 71 70 69 68 67 66 65 64 63 62 61 60 59 58 57 56 55 54 53 52 51 50 49 48 47 46 45 44 43 42 41 40 39 38 37 36 35 34 33 32 31 30 29 28 27 26 25 24 23 22 21 20 19 18 17 16 15 14 13 12 11 10 9 8 7 6 5 4 3 2 1 -2 312 311 310 309 308 307 306 305 304 303 302 301 300 299 298 297 296 295 294 293 292 291 290 289 288 287 286 285 Latitude -4 284 283 282 281 280 279 278 277 276 275 274 273 272 271 270 269 268 267 266 265 264 263 262 261 260 259 258 257 -6 256 255 254 253 252 251 250 249 248 247 246 245 244 243 242 241 240 239 238 237 236 235 234 233 232 231 230 229 -8 228 227 226 225 224 223 222 221 220 219 218 217 216 215 214 213 212 211 210 209 208 207 206 205 204 203 202 201 -10 10 0 350 340 330 320 310 300 Longitude vvvsurvey.org 230 Gb image in the J-band VVV Allsky Map ~500 sqdeg (11 tiles missing) 1pix = 0.4”, total 4x10^10 pix ~223000 images of 512x512 Aladin Ignacio Toledo vvvsurvey.org Year 1 Completeness Maren Hempel VISTA filter transmissions Z Y J H Ks 0.8 1.0 1.2 1.4 1.6 1.8 2.0 2.2 2.4 lambda (microns) DEEPER AND HIGHER RESOLUTION VVV vs 2MASS ZYJHKs Ks<18 JHK Ks<14 SII 9069 SII 9532 HeII 10830 Line emissionw/in filters PaG PaB HeII 14760 Br10 Z Y J H Ks HeI 20581 BrG 0.8 1.0 1.2 1.4 1.6 1.8 2.0 2.2 2.4 lambda (microns) DEEPER AND HIGHER RESOLUTION VVV vs 2MASS Lagoon Nebula (central region) vvvsurvey.org Planetary Nebula VVV field b328 A WORD ABOUT IR PHOTOMETRY . Tricky... because the sky is very bright in the IR. VISTA Dataflow vvvsurvey.org VISTA Telescope Raw Data Acquisition PSO Paranal Science Operations processing CASU Cambridge Astronomical Survey Unit WFAU Wide Field Astronomy Unit VVV Science Team ESO Database VVV OBs vvvsurvey.org YR1: ~2500 OBs - all 152 disk fields observed in 2010A: - multicolor ZYJHKs - Ks 5 epochs - all 196 bulge fields observed in 2010A: - multicolos ZYJHKs - Ks 5 epochs YR2 ~ 5400 OBs - multiepoch Ks band of bulge+disk in 2011A YR3 ~ 15500 OBs - multiepoch Ks band of bulge in 2012A This major activity is carried out periodically. Many details needed to be solved, many problems encountered (skies, concatenations, labeling, etc), this was indeed a huge work. The VVV Survey: Timeline Sky conditions and estimated observing time for the full VVV Survey. Year Time RA range Moon Seeing Transp. Nr of Ks epochs 2010 292h 12:00–19:00 any* 0.8 clear 6 bulge + 6 disk + ZYJH 2011 292h 12:00–19:00 any* 0.8 clear 20 bulge + disk 2012 652h 17:00–19:00 any* any thin 80 bulge 2013 525h 12:00–17:00 any* any thin 70 disk 2014 168h 12:00–19:00 any* 0.8 clear 20 bulge + 9 disk Total 193 nights * The Moon has to be away from the bulge Also constraining airmass to < 2.0 and ellipticity to <0.2 Variable stars vvvsurvey.orgV V V • ~109 stars MACHO variables (Alcock et al. 1998) • ~106 variables RRab δSct (Cepheids) RRc SRs To find RR Lyrae in the bulge To find eclipsing binaries and planetary transits AAA 50 To study rare variable Malargue, sources Sep 2007 Dante Minniti VVV vs. MACHO 10x sqdeg 100x stars vvvsurvey.org Disk Field Combined VLT- optical and VISTA-IR photometry 230 new variables more than expected! Pawel Pietrukowicz 1st VVV RR Lyrae vvvsurvey.org green = 2MASS RR Lyr black = VISTA zone Oscar Gonzalez 1st VVV RR Lyrae vvvsurvey.org OGLE field 30 star 189770 RRab Period = 0.72946 day Amplitude_I = 0.33 mag I = 15.60 V=17.08 V-Imin=1.54 Juan Carlos Beamin A few more RR Lyrae light curves Istvan Dekany A few more RR Lyrae light curves Istvan Dekany A few more RR Lyrae light curves Istvan Dekany A few more RR Lyrae light curves Istvan Dekany A few more RR Lyrae light curves Istvan Dekany A few more EB light curves Istvan Dekany High Energy Sources vvvsurvey.org Follow-up of sources from CHANDRA, INTEGRAL, FERMI, SPITZER, ALMA,... CSO Credit: NASA/UMass/D.Wang et al. VVV will monitor the variability around the Galactic Center. Progress report - observations OK - photometry OK - astrometry OK Some problems / difficulties - low efficiency (shutter open time/total time) - large number of OBs - huge dataset - completeness/homogeneity - large team - delays, delays and more delays - limited dynamic range of detectors VVV In Context vvvsurvey.org 5sigma Point Source Sensitivity (mJy) Sensitivity Source Point 5sigma Valentin Ivanov Area (sqdeg) VVV In Context vvvsurvey.org 5sigma Point Source Sensitivity (mJy) Sensitivity Source Point 5sigma lambda (microns) Valentin Ivanov saturation E Bulge RGC D VVV MS Disk 0.6M+ Bulge RGB Sgr RGC STARS MS Sgr CMD K+M dw Bulge MSTO 4.5 sqdeg b209+b210+b211 photometric limit Roberto Saito qualitative --> quantitative QUALITY CONTROL qualitative quantitative Bright stars vvvsurvey.org Rotation of spider (notice the green, red blue sequence) Detector defects vvvsurvey.org Dead pixels region (in detector Nr. 1) Bright stars vvvsurvey.org CENTAURUS X 10 0 -10 -20 -30 -40 -50 -60 Galactic Longitude Very bright stars present in the VVV fields can cause problems... Bright stars vvvsurvey.org Bright stars not only saturate but also damage the neighboring regions, preventing the recovery of faint stars nearby, and affecting the photometry of neighboring stars. In addition, very bright stars produce bad flat fielding, affecting the whole tile. This is a list of the brightest stars located in the VVV fields. Star Name Equatorial Galactic SpType VisualMag VVVField Alpha Centauri 14 40 -60.8 315.8 -0.7 G2V+K1V -0.29 d052-brightest Ks Beta Centauri 14 04 -60.4 311.8 +1.2 B1III 0.61 d126 Alpha Crucis 12 27 -63.1 300.2 -0.4 B0.5IV+B1V 0.79 d042 Lambda Scorpii 17 34 -37.1 351.8 -2.3 B2IV 1.62 b300 Epsilon Sagittarii 18 24 -34.4 359.2 -9.8 B9.5III 1.84 b207 Kappa Scorpii 17 42 -39.0 351.0 -4.6 B1.5III 2.39 b257-just off edge Upsilon Scorpii 17 31 -37.3 351.3 -1.9 B2IV 2.70 b300?? Delta Sagittarii 18 21 -29.8 3.0 -7.2 K2II 2.72 b238 Lambda Sagittarii 18 28 -25.4 7.7 -6.5 K1III 2.82 b255 Gamma² Sagittarii 18 06 -30.4 0.9 -4.5 K0III 2.98 b278 Iota¹ Scorpii 17 48 -40.1 350.6 -6.1 F2Ia 2.99 b243 Eta Sagittarii 18 18 -36.8 356.4 -9.7 M3.5III 3.10 b205-2nd brightest Lambda Centauri 11 36 -63.0 294.5 -1.4 B9III 3.11 d039?? Eta Scorpii 17 12 -43.2 344.4 -2.3 F3III-IV 3.32 d036-just off edge Bright stars vvvsurvey.org Eta Sgr Flat Fielding vvvsurvey.org Bright stars vvvsurvey.org vvvsurvey.org Year 1 Disk Photometry Roberto Saito, Javier Alonso vvvsurvey.org Year 1 Bulge Photometry Roberto Saito, Javier Alonso Year 1 Astrometry vvvsurvey.org Single epoch, 5 sigma, Vega mag: Z=21.9 Y=21.2 J=20.2 H=18.2 Ks=18.1 Pixel scale: 0.34” Typical image seeing: 1” Best image: 0.6” (including telescope, instrument, seeing) Typical astrometric accuracy (rms per visit) ~35 mas for Ks=15 ~175 mas for Ks=18 Typical proper motion accuracy (after 5yr long survey) ~7 mas/yr for Ks=15 ~15 mas/yr for Ks=18 vvvsurvey.org Multicolor MAPS Reddening Cross-catalogs ASTROMETRY Proper motions Color-magnitude diagrams PHOTOMETRY Color-color diagrams VVV Products Periodic LIGHT CURVES Transients star clusters variables Bulge BDs MW structure CATALOGS Disk TNOs galaxies QSOs OUTREACH Asteroids ~104 vvvsurvey.org TNOs ~102 ASTROMETRY AGNs, QSOs ~103 high-PM ~104 SN ~104 BDs ~104 CVs, Novae ~103 Transients ~105 LMXBs ~103 dM flare ~104 microlensing ~102 5 VARIABLES ~106 WUMas ~3x10 Semidetached ~105 Eclipsing ~5x105 Detached 104 Planetary Transits 103 CATALOGS Ellipsoidal ~104 Periodic RR Lyrae ~104 Spotted ~105 Cepheids ~103 Semiregulars ~104 Pulsating ~105 LPVs, Miras, RCB~103 2 stellar associations ~10 dSct, SXPhe ~104 CLUSTERS open clusters ~103 RVTau ~102 WVir ~102 globular clusters ~10 vvvsurvey.org Not only..
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