Emergency number to Residencia: 1120 THEMIS internal phone: 80, at the end press C/ General remarks on performance: Telescope: excellent Cameras: excellent MTR: excellent TUNIS: excellent Software: excellent Stuff/operators: excellent Network conectivity and speed: good Seeing: poor 24 May 2011, Tuesday ======================= THEMIS operator: Bernard THEMIS people around: Claude, Arturo Weather: cloudy, no observations possible Bernard: MTR spatial scale 0.22 - 0.23 arcsec/pixel - a nice demonstration of application of speckle-reconstruction by Knox-Thomson algorithm (MATLAB implementation) on the THEMIS G-band data Arturo's experiences with velocity determination by Gaussian fit of spectral lines: If both line wings are at the same level (no nearby lines, no blends) one can safely fit with A_0*exp{-z^2/2} + A_3 But if one line wing is higher than another no way to fit it with a slanted Gaussian A_0*exp{-z^2/2} + A_3 + X*A_4 For more see niceday notes. Program: MTR data reduction. Bernard's MATLAB routines. Latter: checking reduced spectra, all OK except 63012 t002_b0505_sp_20110519_09304872_c3.fts still flat field remanents visible (small circles) Reduction done (Bernard): 19 May, 2011 ------------ Sequence 2 (+3) 4554 t002_b0303_sp_20110519_09304872_c3.fts 63012 t002_b0505_sp_20110519_09304872_c3.fts 6497 t002_b0606_sp_20110519_09304872_c3.fts 20 May, 2011 ------------ Sequence 4 4554 t004_b0303_sp_20110520_14051297_c3.fts 63012 t004_b0505_sp_20110520_14051297_c3.fts 6497 t004_b0606_sp_20110520_14051297_c3.fts Sequence 5 4554 t005_b0303_sp_20110520_17350887_c3.fts 63012 t005_b0505_sp_20110520_17350887_c3.fts 6497 t005_b0606_sp_20110520_17350887_c3.fts Sequence 7 4554 t007_b0303_sp_20110520_19011339_c3.fts 63012 t007_b0505_sp_20110520_19011339_c3.fts 6497 t007_b0606_sp_20110520_19011339_c3.fts 23 May 2011, Monday ======================= THEMIS operator: Claude Le Man Morning weather: warm, windless, average seeing sparsed ciruses in height passing accros the sky TUNIS Sequence 1: 1-hour 6563 target: quiet Sun disk center exposure time: 50 ms start: 7:02 UTC (8:02 LCT) duration 1 hour Compensation of solar rotation safely ON. Seeing very changable. Conditions so bad that VTT still closed at 8:45 LCT. Dangerous ciruses at the height. It is almost impossible to say/detect when a cirus could pass in front of the Sun. Take this into account at the analysis. Probably at about 8:50 - 8:55 a clump of ciruses passed accross the Sun just before the end of sequnce. It probably spoiled this sequence. Probably end of sequence can be cut and thrown away. How to guess whether and when a cirus passed: Average each TUNIS particular spectroimage. See time variations of the average - drops should correspond to a pass of cirus. GB context sequence start: 7:41 UTC (8:41 LCT) end: 7:41:50 UTC (8:41:50 LCT) exp time: 4 ms No of shots: 200 time step between shots: 100 ms VDF_2011-05-23_08h41_41.fts TUNIS Sequence 2: 1-hour 6563 target: NOAA 11216 with only one almost symetric sunspot start: 9:58 UTC (10:58 LCT) exposure time 50 ms duration 1 hour Compensation of solar rotation safely ON. Seeing much changable but this observation seemed not to be interfered with ciruses. long, lat (THEMIS control display) 196.18 deg, -15.59 deg CIRUSES at the SUN from about 11:40 to 11:46 LCT !!! Sequnce is spoiled. !!! GB context sequence start: 10:17 UTC end: 10:18:07 UTC exp time: 4 ms No Shots 200 time step 100 ms Afternoon: CLOUDY. NO OBSERVATIONS POSSIBLE ANYMORE. 22 May 2011, Sunday =================== TUNIS free day 21 May 2011, Saturday ======================= THEMIS operator: Rieman Gonzalez Weather: touristic = clear sky, warm, ABSOLUTELY NO WIND bad seeing About noon: total windless Morning: Sequnce 1 TUNIS 4554 target: quiet Sun disk center exposure time 50 ms start: 7:26 UTC (8:26 LCT) duration 1 hour Compensation of solar rotation safely ON. GB context burst: start: 7:34 UTC end: 7:37 UTC exp time: 8 ms No shots: 1000 time step between shots: 200 ms Sequence 2 TUNIS 4554 target: NOAA 11216 (Sunspot with a small tail - future splitting ? ) exposure time 50 ms start: 8:57 UTC (9:57 LCT) duration 1 hour Compensation of solar rotation safely ON. Telscope display coordinates: long, lat 195.69 deg, -15.73 deg p, s 148.5 deg, -683.3 arcsec x,y 205.0 arcsec, -167.8 arcsec from SolarMonitor: S16E16 (-252",-231") from FITS header: LATITUD = -15.7244 LONGITUD = 195.683701 GB context burst: start: 9:25 UTC end: 9:30 UTC (10:29:44 LCT) exp time: 4 ms No shots: 500 time step between shots: 500 ms Sequence 3 TUNIS 6497 target: quiet Sun DC exposure time 50 ms start: 10:31 UTC (11:31 UTC) duration: 1 hour Sequence 4 TUNIS 6497 target: NOAA 11216 (Sunspot with a small tail - future splitting ? ) exposure time 50 ms start: 12:01 UTC (13:01 LCT) duration: 1 hour Telscope display coordinates: long, lat 196.11 deg, -13.82 deg from SolarMonitor: S16E13 (-205",-231") GB context burst: start: 12:16 UTC end: 12:16:47 LCT exp time: 4 ms No shots: 200 time step between shots: 100 ms FoV 120" x 80" Afternoon: exceptionally BAD seeing Izana bathes in warm and humid (40 %) air. NO WIND. OBSERVATIONAL DISASTER. Sparsed clouds in height. No observations in the all afternoon. OBSERVATIONS OF SUNSPOT UMBRAL OSCILLATIONS T. Horn, J. Staude and V. Landgraf Solar Physics Volume 172, Numbers 1-2, 69-76, Compensation of solar rotation on VTT 20 May 2011, Friday ====================== THEMIS operator: Didie, latter Claude came Morning: clear sky but almost no wind, humidity almost 60 % !!! very bad seeing, as usually Didie confirmed: Information about Compensation of the solar rotation doesn't go into fits header. Claud: "Good seeing usually occurred in April, May." Ixon cameras have very good positioning and focusing system. So pixell rows and dispersion are parallel. MTR and TUNIS have different spatial scale. They have to be measured. Some years ago Elena Khomenko experinced an excellent seeing at THEMIS just in May for many days continuously throughout a day. Morning observations: TUNIS oscillations sequences 1 (6563) 2 (6497) 3(4554) Afternoon observations: MTR 3-hour disc center oscillation sequence 1-hour sunspot oscillation sequence 1-hour Evershed flow sequence All at horible seeing 19 May 2011, Thursday ====================== MTR and TUNIS oscillations day ------------------------------- THEMIS operator: Marcel Claude, Arturo: What is a spatial scale of MTR spectra ? Are edges of cameras parallel with direction of dispersion, indeed ? Claude: Put a calibration mask in MTR to measure spatial scale in individual cameras ? EVENT 1: telescope stopped after MTR 2-hours "scan" (not a scan) Sequence 2 and didn't proceed further on FF and DC - after several minutes of waiting I pushed "Stop Observation" trashed the script a continued with "FF" and DC EVENT 2: At the moment of flatfielding an error of dome tracking occurred. Error dome was less than 6 degrees, i.e. error between Solar ephemeris and dome position. Not all FF frames were taken through a clear aperture but through slightly shadowed by dome It means that in FF frames may be seen a trend of decreasing light due to shadowing of the telescope by the dome. Take for flatfielding just FF frames let's say from first ten hadamard loops or FF from a previous sequence (in the worst case). JR, AK: Does VTT have compensation of solar rotation ? What in the case of long multiline observations with a slit perpendicular to the horizon ? Consequences for my PhD Thesis. Angular speed of synodic solar rotation at DC seen from the Earth: 0.15 arcsec/min !!! It means that more than a size of a granule in 10 min. Morning: clear sky, almost no wind, humidity about 20 % seeing: average, not exceptional Solar activity: only two quite circular sunspots at opposite limbs Just two almost circular sunspots at the disk. No well-structured ARs or pores visible. That's why TUNIS sequences taken in the quiet Sun disk center. Purpose/objective: to compare oscillations as seen in MTR and TUNIS interesting thing: Halpha oscillations Morning observations: 1. CALIBRATION SEQUENCE WITH HAIRS start: 9:00, 50 spectra taken (no FF, no DC) at the end two hairs removed from the slit 2. 2-HOUR MTR OSCILLATION SEQUENCE slit: at the disc center (x=0", y=0") oriented along the central meridian of the Sun. Ixon3 (4554) exp 300 ms, accum 10 images, so effective exposure 3 s Ixon5 (63012) exp 50 ms, accum 20 ims, eff exp 1 s Ixon6 (6497) exp 60 ms, accum 20 ims, eff exp 1.2 s Time step between subsequent spectra: 10 s start: 9:20 LCT (8:20 UTC) end: 11:20 LCT Compensation of solar rotation ON all the time. Afternoon observation: Three 1-hour sequences of TUNIS observations in 4554, 6497, 6563 target: quiet Sun disc center exposure time 100 ms 18 May 2011, Wednesday ====================== First data day -------------- THEMIS operator: Claude Morning: west - west-north wind (for the first time from the beginning of the campaign) Morning + Afternoon: high humidity >= 40 % 1. MULTILINE MTR OSCILLATION RUN start: 10:24 end: one hour latter time step: 10 s Exposure times: 4554 300 ms (Ixon3) 6301/2 50 ms (Ixon5) 6497 60 ms (Ixon6) All Ixon cameras start to expose at the same moment but without any latter synchronization. target: QS at disk center Not 100% sure whether compensation of solar rotation was ON. Most probably YES, but it needs a check in telescope log. 1. TUNIS 6497 SEQUENCE start: about 11:46 (not exactly) target: NOAA 11214 (at the west limb) 70 hadamard loops what is approx 30 min than 40 had loops of FF at DC width of scanned area: 14 arcsec height of scanned area: about 80 arcsec end about: 12:19 1. G BAND CONTEXT BURST start at about 11:49 burst finished at 12:05 No of shots: 1000 delay (time step between shots): 1 s exposure time: 6 ms Afternoon ---------- 2-hour MTR oscillation run was interrupted by clouds. Important lecture learned: 1) calibration hairs: put hairs on the slit at the beginning take e.g. 20 spectra with them then remove hairs away to avoid latter clipping of the spectra, the full with of the spectra can be used difficult flatfielding of the spectra with hairs 2) accumulation mode (i.e. in-camera summing of spectra): results in better signal to noise ratio - good for studying of oscillation Ixon3 (4554) exp 300 ms, accum 10 images, so effective exposure 3 s Ixon5 (63012) exp 50 ms, accum 20 ims, eff exp 1 s Ixon6 (6497) exp 60 ms, accum 20 ims, eff exp 1.2 s Time step 10 s set in the script will be kept also in accum mode. No need to modify it. 3) Slit position and orientation: at the disc center along central meridian of the Sun. It means that the differential refraction can not be compensated, but it can be negligible in oscillation obs in average seeing at THEMIS. 4) Rotation Soleil Compensee: be sure that it is ON. Canarian Summer Time = UTC + 1 hod THEMIS Latitude = 28 deg 18' 13.8'' N Longitude = 16 deg 30' 31.6'' W Altitude = 2456 m 17 May 2011, Tuesday ==================== TUNIS and GB practice day -------------------------- Time of arrival (departure) to (from) the telescope: 8:30 - THEMIS people around: Marcel, latter Bernard and Claude Weather: south - south-west circulation persists (see movie in gallery) warm, very bad seeing "Something-is-better-than-nothing" strategy is adopted for the rest of campaign. GB - camera: Maximum No of shots allowed: 1000 ff at FLAT.fts Test burst 1: VDF_2011-05-17_09h35_46.fts No of shots: 1000 delay (time step between shots): 200 ms exposure time: 4 ms approx burst duration: (4 + 200)*1000 = 204 s = 3.4 min Start at about: 9:35 End at: 9:38:07 ssh obs281@observador.themis.iac.es cd /data/themis/ Time is always in local Canarian time. Afternoon: 30-min TUNIS test run to estimate data volume raw TUNIS data 1.1 GB FF 621 MB DC 18 MB Important lecture: PLACE A PORE PREFERENTIALLY OUT OF AREA SCANNED BY HADAMARD MASK 16 May 2011, Monday =================== TUNIS practice day ------------------ Weather Morning: clouds from the East, warm, south wind Bernard says these are unusually bed conditions for this season. very bad seeing THEMIS people around: Didie, latter Bernard Action/Program: Didie+Bernard solve network problems in communication between IO comp and a master telescope computer. IO comp doesn't receive pointing coordinates from the master. Due to clouds and very bad seeing no observation are thinkable (luckily). So no much lost. Comp problems solved and we did test TUNIS observations in 4554, 6497, and Halpha along with saving G-band context images from the THEMIS pointer. Important note: - time step between two subsequent positions of Hadamard mask: 600 - 700 ms !!!! - very slow in the term of how much seeing changes in 600 - 700 ms - this is the reason black-and-white rims of sunspot seen in the Sequence 5 from May 14 - the time step should much improve with the new positioning motor of the Hadamard mask - DON'T FORGET: - stop QuickLook of camera before: - modification of wavelength in Camera config tab - starting of the observation Time of arrival (departure) to (from) the telescope: 8:00 - 19:30 No real observations taken. 15 May 2011, Sunday =================== THEMIS free day ---------------- Morning: phototrip at Izana Observatory Afternoon: Volcan de Fasnia round trip, Sendero No. 20 whole-afternoon trip, very nice, recommendable http://senderosdemitierra.blogspot.com/2009/03/tenerife-volcan-de-fasnia-sendero-n-20.html 14 May 2011, Saturday ==================== TUNIS practice and data reduction day ------------------------------------- weather: clear sky in the morning, calima receded latter clouds raised up very bad seeing south wind Morning: TUNIS practice, taken data at 4554 Afternoon: on-the-fly writing software for TUNIS data reduction 4554 Arturo's routines: had3.pro, had_geom.pro for demultiplexing TUNIS data Arturo: an entrance window bellow hadamard mas was made 1.5 micrometer wider than it should be, this is as Hadamard mask had 32 slits instead of 31 - already included in reduction code as a pseudodemultiplexing Time of arrival (departure) to (from) the telescope: 8:00 - 20:00 THEMIS people around: Bernard, Arturo Miscellaneous: - MTR/TUNIS filename convention: y - FF x - DC b - raw data r - reduced data MTR slit width: 0.5 arcsec MTR camera exposure times (same for obs, ff, dc): 4554 300 ms 6301/2 60 ms 6497 70 ms TUNIS camera exposure time: 6497 50 ms (or between 50 and 150 ms), saturates at 200 ms PC IO /home/themis/koza_tunis.txt Duration of a particular TUNIS run at 4554 10 hadamard loops then 10 ff images of 40-ms exp time then dc in total: 11 min from that: 4 min 15 s hadamard 10 loops itself the rest ff and dc TUNIS time resolution: 4 min 15 s = 255 s --> 25.5 s per 1 hadamard loop The same in other way: WACQ (acquisition): 80 ms (50 ms exposure + 30 ms communication etc.) JOG (poskocenie posununutie): 600 - 700 ms i.e. 31*(650 + 80) = 22.5 s WIDTH OF TUNIS SCAN: 14 arcsec height of TUNIS window: about 70 arcsec (after cutting upper and lower wedge) Tunis spatial scale (pixel size): about 0.2 arcsec/px 4554 TUNIS dispersion: about 9 mA/px G-BAND DISPLAY: info about FoV: 120" x 80" display ??? size of image in FITS ??? No real observations taken. 13 May 2011, Friday ==================== Technical day ------------- weather: cloudless, warm calima still persists = means very bad seeing the all day Morning: - learning and practicing MTR operation - test data taken in 4554, 6301/02, 6497 Afternoon: - learning how to operate TUNIS, test data taken in 6497 - brief intro into reduction of MTR and TUNIS data - example velocity and intensity maps produced from MTR test data by Arturo's routines Time of arrival (departure) to (from) the telescope: 8:00 - 20:00 Important lecture: DON'T FORGET TO ROTATE MANUALLY TUNIS FILTER WHEEL WHEN SWITCHING FROM 4554 TO 6563 OR 6497 DON'T TOUCH BY FINGERS THE FILTERS SINCE EXP. TIME OF TUNIS CAMERA IS ONLY 50 ms MORE THAN 20 FF IMAGES ARE NEEDED TO WASH OUT THE SUN ALWAYS KEEP THE SEQUENCE: SCAN(OBS) - FF - DC No real observations taken. THEMIS people around: Claude, Arturo, Bernard Guests in lunchtime: Javier Trujillo Bueno with his student from Trente Andres Asensio Ramos with Maria (at VTT in that time)