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| Here is the full detailed formatted list [[attachment:Source_list_fmt2013v2.txt|Full list]] with fluxes | Here is the full detailed formatted list [[http://www.iram.fr/wiki/nika2/images/8/85/Source_list_fmt2013v3.txt|Full list v3]] with fluxes |
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| Here is the catalog for Pako [[attachment:NIKA2013v2.sou.txt]] has to be RENAMED to NIKA.sou on the pako computer | Here is the catalog for [[http://www.iram.fr/wiki/nika2/images/b/bb/NIKA2013v3.sou.txt|Pako]] has to be RENAMED to NIKA2013R6.sou on the pako computer (DONE) |
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| ------------------------------------ To be Written ------------------------------------------------------------- | |
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| Short manual on useful "Pako for Nika" commands: NEW (14/11/12, 18/11/12 SL) [[attachment:Pako_helpv14.txt]] | Short manual on useful "Pako for Nika" see on Granada computers 2013_docs_for_observations/Pako_helpv15.txt |
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| NEW (12/11/12, SL): Hans' memo about the Tones tuning scripts in Pako: [[attachment:ncs30mProjectsPlanningNIKA.pdf]] Here is a collection of Pako scripts to gain time and have a reference on the observations we will do (to use them rename the files without the .txt, 2nd version updated with slower mapping speed to minimize tracking errors, 3rd version include pako line continuation sign (-)): NEW (17/11/12, SL): [[attachment:Maximum_OTF_speed_vs_Elevation.txt]] => a table showing the maximum velocities possible for the scans for various elevations. NEW (14/11/12, SL) init file for pako: ini.pako automatically loaded with the pakoNIKA command; the old nini.pako -renamed as nin_OLD.pako- is deprecated and will cause errors if loaded. [[attachment:ListAstroTargetNika3/OTF_pointing.pako]] => OTFMAP 100"x84" in 22 subscan x 10 s = 4+1 ~= 5 min (10"/s) with 2.6 samples (subscan step) per convolved 1mm HPBW (for pointing & focus). 10s = minimum subscan time possible (Pako doesn't authorizes less), hence the choice of subscan length. Scan height changed from 60" to 92" to have more margins for the useful pixels. [[attachment:ListAstroTargetNika3/OTF_geometry.pako]] => OTFMAP 300"x220" in 56 subscan x 20 s = 19+3 ~= 22 min (15"/s) with 2.6 samples (subscan step) per convolved 1mm HPBW (for the array geometry = pixels map in sky) [[attachment:ListAstroTargetNika3/OTF_ps.pako]] => OTFMAP 140"x90" in 19 subscan x 14 s = 4+1 ~= 5 min (10"/s) with 2 sample (subscan step) per convolved 1mm HPBW (for point source observations) [[attachment:ListAstroTargetNika3/OTF_2x2.pako]] => OTFMAP 120"x120" in 25 subscan x 12 s = 5+1 ~= 6 min (10"/s) with 2 samples (subscan step) per convolved 1mm HPBW (for extended source < 2') [[attachment:ListAstroTargetNika3/OTF_5x5.pako]] => OTFMAP 300"x300" in 51 subscan x 20 s = 17+3 ~= 20 min (15"/s) with 1.7 samples (subscan step) per convolved 1mm HPBW (for extended source < 5') [[attachment:ListAstroTargetNika3/OTF_10x10.pako]] => OTFMAP 600"x600" in 41 subscan x 30 s = 20+4 ~= 24 min (20"/s) with 0.7 samples (subscan step) per convolved 1mm HPBW (for very extended source < 10') [[attachment:ListAstroTargetNika3/OTF_faint_source.pako]] => OTFMAP 120"x80" in 21 subscan x 12 s = 4.2+0.8 ~= 5 min (10"/s) with 2.6 samples (subscan step) per convolved 1mm HPBW (for faint sources) [[attachment:ListAstroTargetNika3/OTF_deep_field.pako]] => OTFMAP 360"x360" in 61 subscan x 20 s = 20+4 ~= 24 min (18"/s) with 1.7 samples (subscan step) per convolved 1mm HPBW (for faint sources) [[attachment:ListAstroTargetNika3/OTF_sz.pako]] => OTFMAP 360"x240" in 41 subscan x 20 s = 14+3 ~= 17 min (18"/s) with 1.7 samples (subscan step) per convolved 1mm HPBW (for faint sources) [[attachment:ListAstroTargetNika3/OTF_moon.pako]] => OTFMAP 2000"x 2000" in 34 subscan x 40 s = 23+3 ~= 26 min with 0.17 samples (subscan step = 60) per convolved 1mm HPBW (to look at the moon in bad weather) NEW (18/11/12, SL): [[attachment:diy-test-00.pako]] => 11 sec scan at (440";330") off-source (equivalent to TRACK with an offset) sending a specific key word for tuning [[attachment:diy-test-03.pako]] => equivalent to a 800"x700" OTF, but with 10 sec pause between each subscan and sending a specific key word for tuning [[attachment:diy-test-12.pako]] => equivalent to tip, between 1.1 and 3.5 airmasses with 6 steps of 0.4 airmass, including a 11 sec pause followed by 22 sec integration, and sending a specific key word for tuning between each step of the sky dip. [[attachment:OTF_geom_below70degEl.pako]] => OTFMAP 420"x 220" (step 4) in 56 subscans x 12 s = 11+3 ~= 14 min (35"/s) with 2.6 samples (subscan step) per convolved 1mm HPBW (for the array geometry = pixels map in sky: much faster than previous OTF_geometry, while keeping oversampling the diffraction pattern; guarenteed to work well below 70 degrees elevation. [[attachment:OTF_faint_source_Az.pako]] => OTFMAP 120"x 90"(step 6) in 16 subscan x 10 s = 3+1. ~= 4 min. (12"/s) with 2 samples (subscan step) per convolved 1mm HPBW (for faint sources, slightly different that OTF_faint_source.pako), subscan in Azimuth, steps in Elevation [[attachment:OTF_faint_source_El.pako]] => same as previous one, except that subscans are in Elevation, steps in Azimuth [[attachment:OTF_faint_source_RA.pako]] => same as previous one, except that subscans are in Right Ascension, steps in Declination [[attachment:OTF_faint_source_Dec.pako]] => same as previous one, except that subscans are in Declination, steps in Right Ascension [[attachment:OTF_10x10_faster_Az.pako]] => OTFMAP 600"x 600" (step 15) in 41 subscan x 20 s = 14+5 ~= 19 min. (30"/s) with 0.7 individual pixel sample (subscan step) per convolved 1mm HPBW (slightly different that OTF_10x10.pako), subscan in Azimuth, steps in Elevation [[attachment:OTF_10x10_faster_El.pako]] => same as previous one, except that subscans are in Elevation, steps in Azimuth Here's an excel sheet which helps to find the best focus thanks to a 2nd order polynomial line trend fitting on beam width and amplitude (note that amplitude is much more robust): [[attachment:ListAstroTargetNika3/Focus.xls|Full focus Excel only]], [[attachment:ListAstroTargetNika3/BestFocus.ods|Best focus with basic 2nd order polynomial]] ---- == Real Time Analysis == New (12/11/12, SL): Xavier's and Robert's memo to start real time Mopsic analysis: [[attachment:HelpMopsicSecurForWiki.txt]] (there is also a README in the directory, where the pointings & foci should be processed) Userl Manual for the Real time analysis: [[RealTime_User_Manual |User Manual RTAnalysis]] ---- == Recommandations for the Pointing Sessions == - NEW (18/11/12, SL). Available pointing sources are displayed on Xephem, together with Antenna position.The default catalogues loaded are NIKA2012R5.edb and pointing_sources.edb. The later display fluxes as "_mK" appended to the source name, but the coordinates are in J1950; to avoid confusion delete pointing_sources.edb, and load instead pointingIRAM30m.edb showing all the pointing source of the IRAM data base and NIKA_StrongPointSources.edb, which gather the 20 strongest sources with indicative (few years old) fluxes @ 2mm appended to the names; both catalogues are in J2000 and the symbols are proportional to the flux. - NEW (18/11/12, SL). The pointing source catalogue to use in PaKo is iram-J2000.sou; it is identical to pointingIRAM30m.edb expect that if loaded in Xephem the sources appear with the default symbol which is used in the NIKA2012R5.edb catalogue |
- Pako scripts are in the Pako subdirectory |
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| - If a source is available both at low and high azimuth, use command SET TOTO LOW (or SET TOPO HIGH) to stay on the source without moving. | - If a source is available both at low and high azimuth, use command SET TOPO LOW (or SET TOPO HIGH) to stay on the source without moving. |
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=== Abstract === |
|
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| Pointing (Cross), Focus, OTF_Geometry, Skydip, Lissajou, OTF_Map. Tests include tuning, auto-tuning, robustness of data acquisition. Photometric calibration includes planets and secondary calibrators. Skydip and Lissajou sequences need to be better tested than before. Other sequences should be straightforward. | Pointing (Cross), Focus, OTF_Geometry, Skydip, Lissajous, OTF_Map. Tests include tuning, auto-tuning, robustness of data acquisition. Photometric calibration includes planets and secondary calibrators. Skydip and Lissajous sequences need to be better tested than before. Other sequences should be straightforward. The plateau systematics will be investigated via the OTG_geometry sequences. Near sidelobes can be measured by doing 5x5 map of of Jupiter or Saturn and use Pf variable. === Detailed version (after discussions SL, FXD, RZ, NB, AB, AS, HU) === * Alignment with laser. Then align mm axis by minimizing the background (manual rotation) * Nominal mode is 8Hz. * One OTF_geometry to have an idea of the Focal Plane Geometry. Decide on a reference pixel at 2mm (with a close 1mm counterpart) so as to avoid problems with weather * A reasonable pointing session to start with. A least 15 sources spread on the local sky (see above). No offset corrections starting with zero nasmyth offsets, nor azel offsets. Pointing should be done with a cross followed by a Lissajous (could be the nominal mode soon). * Focus: Standard one AND/OR 3 Lissajous scans with 3 different focus values AND/OR 3 OTF_geometry with 3 different focus values. Lateral focus could be tried once. * Photometric and FPG calibration with OTF_geometry on planets or strong quasars: get a first idea of flux calibration, FWHM, Kid positions * Skydips. Needed only to calibrate the total power measurements: 2 (down up) at the beginning and 2 at the end of one session * Photometric calibration on Primary and secondary calibrators with Lissajous scans * Faint point source measurement (for a source with a known position (at the center)). Lissajous scans for several hours. * Deep field 3x3 arcmin field in Az or El zigzag mode (point sources are looked for with unknown flux and position) * Extended sources: e.g. M82, Gal. Sources, Crab, CasA: try various speeds to retrieve large angular scales: 10, 20,30,40,50,60 arcsec/s in zigzag Az, El mode * SZ mapping: same |
| Line 168: | Line 130: |
| We have a total of 85 hours. About 12 hours for 7 days. Subtracting the 40 hours for commissioning, we are left with 45 hours. Taking out 15 hours for calibration (calibration on planets and secondary calibrators, pointing, focus, skydip), we are left with 30 hours of science scans, which we spread this way, with the sources in order of priority: | We have a total of 85 hours. About 12 hours for 7 days. We dedicate 40 hours for commissioning, 45 hours are left for 5 scientific programs (Rho Oph, M33, HSO extragalactic sources, Deep survey and RXJ). Taking out 15 hours for calibration (calibration on planets and secondary calibrators, pointing, focus, skydip), we are left with 30 hours of science scans. The sources to be used during commissioning and science are the same. |
| Line 170: | Line 132: |
| 1. Dense Galactic regions (4h) 2. Rho Oph (6h) 3. Extended galaxies (4h) NGC891 4. Faint sources (7h) 5. Deep survey (4h) 6. Clusters of galaxies (5h) RXJ |
1. Rho Oph (6h) 2. Extended galaxies (8h) M33 3. Faint sources (7h) 4. Deep survey (4h) 5. Clusters of galaxies (5h) RXJ |
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| Here is a priority list of targets (see the complete list above). | Here is a priority list of targets (see the complete list above) for commissioning and science observations. |
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| 2.5. NGC891 | 2.2. M33 2.3. NGC891 |
| Line 193: | Line 155: |
| Arp220, 4C05.19, APM08279+5255, MM18423, SMMJ2135, HAT083051, HAT113526, HAT114637, HAT133008, HSO_ID141, HAT133649, HAT134429, HAT141351 | Arp220, 4C05.19, APM08279+5255, MM18423, SMMJ2135, HAT133008, , HAT133649, HAT141351 |
| Line 195: | Line 157: |
| HATLENS01, HATLENS02, HATLENS03 (=HAT114637), HATLENS04, HATLENS05 (=HSO_ID141), HATLENS06 (=HAT134429), HATLENS07 (=HAT083051), HATLENS08, HATLENS09 (=HAT113526) |
Useful information for observations: List of astronomical Target, Pako scripts, Real Time Analysis, Observing strategies
Contents
List of Astronomical Target for Nika June 2013 run6
FXD: First version (2 May 2013)
1. Planets
Mars, Uranus, Neptune for photometric calibration (primary calibrators) and focal plane geometry.
(Venus, Jupiter, Saturn) too hot too big
Name |
Right Ascension |
Declination |
Size (arcsecond diameter) |
Flux @ 1.25 mm |
Flux @ 2.05 mm |
MARS |
04:25:09.5231 |
21:50:15.451 |
3.80x3.78 |
95.3 Jy |
32.8 Jy |
URANUS |
00:45:14.8752 |
04:06:50.511 |
3.44x3.33 |
47.2 Jy |
16.4 Jy |
NEPTUNE |
22:29:43.1041 |
-10:09:06.590 |
2.26x2.20 |
19.4 Jy |
6.72 Jy |
Here are the ephemeris for all planets The near and far sidelobes could be measured with Jupiter and Saturn.
2. Usual bright quasars
- for image quality, linearity checks, and pointing sessions
3. Secondary Calibration sources Calibrator galactic sources Here is IRAM report on Secondary Calibrators
4. Strong Galactic sources to test mapping Strong galactic sources
5. Weak Galactic sources
- for photometric calibration checks
6. External extended galaxies
- for Science demonstration (mapping)
7. High redshift sources
- for Science demonstration (sensitivity)
8. Hatlas lens sources
- for Science demonstration (sensitivity)
9. Deep survey and SZ sources
- for Science demonstration (SZ sensitivity)
Deep survey and cluster of galaxies
Here is the full detailed formatted list Full list v3 with fluxes
Here is the catalog for Pako has to be RENAMED to NIKA2013R6.sou on the pako computer (DONE)
Here is a list of IRAM pointing sources with fluxes at 3mm and 2mm (I miss fluxes at 1mm, SL) FluxForPointingSources
Interface with the telescope: Pako
Short manual on useful "Pako for Nika" see on Granada computers 2013_docs_for_observations/Pako_helpv15.txt
- Pako scripts are in the Pako subdirectory
- Before starting the pointing session, we may be requested to move the azimuth by 60deg to reset the inclinometer of the az axis.
- Always stay at more that 1 deg from the Sun. There are internal safeties that prevent the antenna to point to the Sun, but we may not get error messages.
- try to get sources uniformly distributed on the sky, hence give priority to high elevation sources that are usually harder to reach.
- Do one focus at the beginning. No need to do more focus than one every 2-3hours.
The antenna can point between 60 and 460 degrees in azimuth, between 20 and 80 degrees in elevation.
- If a source is available both at low and high azimuth, use command SET TOPO LOW (or SET TOPO HIGH) to stay on the source without moving.
- The minimum number of sources to observe for the pointing model is 15. 30 is good enough.
- the pointing sources should be observed on 'short' period, e.g. 3-4 hours to avoid daily pointing variations
Commissioning requirements
Abstract
We can consider using 40 hours to test, calibrate and commission the instrument. Procedures will be tested several times, which include Pointing (Cross), Focus, OTF_Geometry, Skydip, Lissajous, OTF_Map. Tests include tuning, auto-tuning, robustness of data acquisition. Photometric calibration includes planets and secondary calibrators. Skydip and Lissajous sequences need to be better tested than before. Other sequences should be straightforward. The plateau systematics will be investigated via the OTG_geometry sequences. Near sidelobes can be measured by doing 5x5 map of of Jupiter or Saturn and use Pf variable.
Detailed version (after discussions SL, FXD, RZ, NB, AB, AS, HU)
- Alignment with laser. Then align mm axis by minimizing the background (manual rotation)
- Nominal mode is 8Hz.
- One OTF_geometry to have an idea of the Focal Plane Geometry. Decide on a reference pixel at 2mm (with a close 1mm counterpart) so as to avoid problems with weather
- A reasonable pointing session to start with. A least 15 sources spread on the local sky (see above). No offset corrections starting with zero nasmyth offsets, nor azel offsets. Pointing should be done with a cross followed by a Lissajous (could be the nominal mode soon).
- Focus: Standard one AND/OR 3 Lissajous scans with 3 different focus values AND/OR 3 OTF_geometry with 3 different focus values. Lateral focus could be tried once.
- Photometric and FPG calibration with OTF_geometry on planets or strong quasars: get a first idea of flux calibration, FWHM, Kid positions
- Skydips. Needed only to calibrate the total power measurements: 2 (down up) at the beginning and 2 at the end of one session
- Photometric calibration on Primary and secondary calibrators with Lissajous scans
- Faint point source measurement (for a source with a known position (at the center)). Lissajous scans for several hours.
- Deep field 3x3 arcmin field in Az or El zigzag mode (point sources are looked for with unknown flux and position)
- Extended sources: e.g. M82, Gal. Sources, Crab, CasA: try various speeds to retrieve large angular scales: 10, 20,30,40,50,60 arcsec/s in zigzag Az, El mode
- SZ mapping: same
Science case demonstration
We want to show typical science demonstration data in five areas where we can compare our results with previous (Mambo, Laboca, JCMT, Bolocam) bolometer array results. We have a total of 85 hours. About 12 hours for 7 days. We dedicate 40 hours for commissioning, 45 hours are left for 5 scientific programs (Rho Oph, M33, HSO extragalactic sources, Deep survey and RXJ). Taking out 15 hours for calibration (calibration on planets and secondary calibrators, pointing, focus, skydip), we are left with 30 hours of science scans. The sources to be used during commissioning and science are the same.
- Rho Oph (6h)
- Extended galaxies (8h) M33
- Faint sources (7h)
- Deep survey (4h)
- Clusters of galaxies (5h) RXJ
Here is a priority list of targets (see the complete list above) for commissioning and science observations.
- Galactic regions, From brighter to fainter TBD
- 1.1. Large map of OrionLBS23SM 1.2. Large map of DR21 1.3. Large map of Crab, CasA 1.4. Map of NGC2023 1.5. Map of the horsehead
- Galactic faint sources: Rho Oph
- Extended galaxies
- 2.1. M82 2.2. M33 2.3. NGC891
- Faint high-z point sources starting with 30 mJy sources at 1mm TBD:
- Arp220, 4C05.19, APM08279+5255, MM18423, SMMJ2135, HAT133008, , HAT133649, HAT141351 H1413+517, F10214+4724, HLSW01, BR1202-0725, BRI1335-0417, SBS1408+567, , HSO_ID017, HSO_ID081, HSO_ID011,HSO_ID130.
HATLENS01, HATLENS02, HATLENS03 (=HAT114637), HATLENS04, HATLENS05 (=HSO_ID141), HATLENS06 (=HAT134429), HATLENS07 (=HAT083051), HATLENS08, HATLENS09 (=HAT113526)
- Deep survey: The idea is to cover a field with 1mJy rms sensitivity at 1mm and 0.5mJy at 2mm, this is about one hour per camera FOV (about 3 arcmin^2). Map should be 3x4 arcmin. Exact field to be decided around a faint source (5-10 mJy)
- Clusters of galaxies RXJ1347-1145, Confirm