DST

DST

From

Sac Peak DST (1969 -- )VTT (1989 -- ) & GREGOR (201X --)SST (2002 -- )BBSO: NST (1969, 2008 -- )

Hida DST (1979 -- ) Sacramento Peak, National Solar ObservatoryRichard B. Dunn Solar Telescope (DST)

Sacramento Peak, National Solar ObservatoryRichard B. Dunn Solar Telescope (DST)

41.5m

25067m

Solar Adaptive Optics ProjectSince the late 1990s the National Solar Observatory has been advancing the Shack-Hartmann technique. We divide the solar image into subapertures then deform a flexible mirror so each subaperture matches one reference subaperture. In 1998 we applied a low-order AO system to the Dunn Solar Telescope, thus allowing it to operate near its diffraction limit under moderately good atmospheric conditions. This technology now is applied at several solar telescopes around the world.

Sacramento Peak, National Solar ObservatoryRichard B. Dunn Solar Telescope (DST)Sacramento Peak, National Solar ObservatoryRichard B. Dunn Solar Telescope (DST)Instruments for imaging

A unique instrument at the focus of the Dunn Solar Telescope is theUniversal Birefringent Filter, or UBF. (Lyot type filter with rotating crystal elements using quarter waveplates and linear polarizers to tune.) It can be tuned to look at any particular visible color in the Sun's spectrum. A picture can then be taken of that region of the sun. This allows scientists to observe different altitudes and temperatures on the sun, as each chemical element emits or absorbs its own color of light.

In order to record images or spectra, an electronic camera called a CCDis often used. The pictures are read by a computer and stored either on disk or magnetic tape for later analysis.Sacramento Peak, National Solar ObservatoryRichard B. Dunn Solar Telescope (DST)Instruments for imagingIBIS: Interferometric Bidimensional Spectrometer

The Interferometric Bidimensional Spectrometer (IBIS) is a Solar Research Instrument on the DST.2

Sacramento Peak, National Solar ObservatoryRichard B. Dunn Solar Telescope (DST)Instruments for spectroscopyHSG: the Horizontal Spectrograph TheHorizontal Spectrograph(HSG) is a high spectral and spatial resolution instrument. The spectrograph consists of a rectangular slit, of fixed width, a collimator lens, plane grating, camera lenses, and CCD detectors.

Component Description Grating: 316 lines/mm reflection type by Bausch and Loumb 206mm x 128 mm ruled area Blazed at 63.4333 degrees (63 degrees, 26 minutes) Blaze wavelength - all Resolution 472,596 (2/3 of theoretical) at 5000 A, 11th order, resolving power 7mA Slit: Adjustable Scale at slit = 7.5arcsec/mm, Maximum FOV = 170 x 170 arcsec 1 arcsec = 133.3 microns Collimating Lens: 3 meter focal length for f36 setup, 1.5 meter focal length for f72 Camera Lenses: 3 meter focal length singlets or 1.5 meter focal length singlets

Sacramento Peak, National Solar ObservatoryRichard B. Dunn Solar Telescope (DST)Instruments for spectroscopy 4

Advanced Stokes Polarimeter (ASP) : This uses a horizontally-mounted spectrograph to study complex magnetic fields, such as are common in sunspots. The ASP can also be used with the UBF to produce simultaneous, coordinated data sets.Cf. Elmore et al. 1992 SPIE, 1746, 22ESacramento Peak, National Solar ObservatoryRichard B. Dunn Solar Telescope (DST)Instruments for spectroscopy

TheDiffraction-Limited Spectro-Polarimeter(DLSP) built in collaboration with the HAO and operated at the NSO Dunn Solar Telescope is an innovative and contempo grating polarimeter specifically designed to meet the high requirements pursued in solar spectropolarimetry. With the excellent imaging properties of the instrument and the efficient performance of the high-order adaptive optics system we achieve a spatial resolution of 0.4 arcsec on a regular basis.The spectrograph is in an autocollimated configuration (Littrow mount) with an off-axis parabola (P). The dispersive element is a 79 grooves/mm Echelle grating (G) working in high order (36th order). The aperture slit (S) has a width of 12 micron. The detector (CCD) is a high speed, backside illuminated split-frame transfer sensor (652 x 494 pixel) manufactured by PixelVision.The DLSP uses two ferro-electric liquid crystals upfront right after the exit port to modulate the light beam. A polarizing beam splitter (PBS) right in front of the detector acts as an analyzer.Sacramento Peak, National Solar ObservatoryRichard B. Dunn Solar Telescope (DST)Instruments for spectroscopyThe DLSP has two operation modes coined high- and low-resolution mode. In high resolution the diffraction limit of the DST @630.2 nm is critically sampled with 0.09 arcsec/pixel covering 59 arcsec along the slit. In low resolution the spatial sampling is 0.25 arcsec/pixel allowing for a larger FOV of 163 arcsec.

Sacramento Peak, National Solar ObservatoryRichard B. Dunn Solar Telescope (DST)Instruments for spectroscopyFIRS: the Facility IR SpectropolarimeterTheFacility Infrared Spectrapolarimeterfor the Dunn Solar Telescope is an advanced imaging spectropolarimeter developed by the Institute for Astronomy - University of Hawai'i (P.I. Haosheng Lin) and the National Solar Observatory. This instrument provides simultaneous spectral coverage at visible and infrared wavelengths through the use of a unique dual-armed spectrograph design. The geometry of the spectrograph has been specially designed to capture the Fe I 6302 and 15648 lines with maximum efficiency. In addition, the spectrograph operates in a multiple slit mode. By using narrow band filters, the spectra from four consecutive slit positions can be imaged at once on the same detector. This feature greatly reduces the time necessary to scan across a large area on the sun, making it an ideal instrument for the study of quickly developing active regions.

Sacramento Peak, National Solar ObservatoryRichard B. Dunn Solar Telescope (DST)Instruments for spectroscopySPINOR: Spectro-Polarimeter for Infrared and Optical RegionsSPINOR is an instrument developed for the NSO by HAO.

Polarization OpticsAll the optical mounts built for theAdvanced Stokes Polarimeterare used for SPINOR as well. Every ASP optical element is replaced by a new achromatic one.

Entrance Window Calibration PolarizerThe entrance window calibration polarizer is an array of 13VersaLightwafers. The wafer diameter is approximately 150mm (with a flat on one side aligned to the polarization direction). The mechanical mount developed for DST calibration that fits over the entrance window of the telescope has been modified to accept theseachromatic Versalight polarizers.

Calibration Linear PolarizerThe calibration linear polarizer is VersaLight selected for good performance over a 50mm aperture and AR coated for 450nm to 1600nm. The location of the calibration Linear polarizer is the stage closest to the exit port of the telescope in the Calibration Modulation Unit.

Calibration RetarderThe calibration retarder is a 50mm diameterbi-crystalline achromatof the design shown in the plot, but with thicknesses scaled for quarter wave retardance between 450nm to 1600nm and AR coated for the same range. The location of the calibration retarder is the stage just above the calibration linear polarizer in the Calibration Modulation Unit where the light beam is f/72.Sacramento Peak, National Solar ObservatoryRichard B. Dunn Solar Telescope (DST)Instruments for spectroscopySPINOR: Spectro-Polarimeter for Infrared and Optical Regions

Polarization ModulatorThe polarization modulator is a 50mm diameterbi-crystalline achromatwith thicknesses scaled for0.35 wave retardancefrom 450nm to 1600nm and AR coated for the same range. The location of the polarization modulator is just after the fast mirror near the exit of the Calibration Modulation Unit where the beam is f/36. This retarder design includes positive and negative birefringent crystals has a low variation ofretardance vs. angle. It is likely that the temperature will need to be monitored as there is a small variation ofretardance vs temperaturethatdiminishes with wavelength.Polarizing Beam SplitterThe polarizing beam splitter uses a VersiLight beam splitting cube, is 16.5mm per side and is the same design as that developed for the ASP. As with the ASP, the image of the slit is split into two beams separated vertically. Each beam is polarized at 45to the orientation of the rulings on the grating. The polarizing beam splitter is just behind the entrance slit of the Horizontal spectrograph.GratingsSince SPINOR operates over a much wider wavelength range compared to ASP, different grating choices are appropriate. Depending upon the spectral line of interest and spectral resolution desired different gratings might be selected. Higher blaze angle gives higher spectral resolution for the same spatial sample size. Since SPINOR will operate with AO, its design should tend towards higher spatial resolution than the ASP, but since it is a research instrument and cannot be optimized for a single line, not as high as DLSP. Thesespectrograph issueslead to a spectrograph using a 40mm slit and 1000mm camera lens.The Infrared Triplet is of special interest for SPINOR as the three lines are inaccessible to ASP both due to the calibration optics and the performance of the 316 line/mm grating at these wavelengths. Four possibleSPINOR gratingshave good performance for near infrared lines.Teide Observatory, TenerifeVacuum Tower Telescope (VTT)

It is operated under the leadership of the KIS (60%) in cooperation with AIP (20%) and MPS (20%). It is a classical solar telescope: two celeostat morrors feed the sunlight into the telescope. It has a 70 cm diameter primary mirrorand afocal lengthof 46 m. Thanks to anadaptive opticssystem, in operation since spring 2000, it is able to resolve details down to 0.2 arcsec.38mTeide Observatory, TenerifeVacuum Tower Telescope (VTT)- Diameter of primary mirrorl: 70 cm- Focal length: 45.640 m- Aperture ratio f/D: 65.7- Resolving power at 543.4 nm: 0.196"- Image scale in primary focu: 4.59"/mm

Teide Observatory, TenerifeVacuum Tower Telescope (VTT)An adaptive-optics system Is permanently installed and available to all instruments; this leads to a substantial improvement of the image quality. On good days, this provides a spatial resolution of about 0.2 arcsec at 500 nm for short exposures, and of some 0.5 arcsec for exposures as long as 10 seconds.

35 actuators, 50mm illuminated pupil diameter, 100mm total diameter- Minimum radius of curvature (maximum voltage (400V) applied to all actuators): ca 20m- First resonance frequency: 900 HzInstruments for ImagingTeide Observatory, TenerifeVacuum Tower Telescope (VTT)TESOS/VIP is a 2D spectrometer based on three Fabry-Perot interferometers with a telecentric design and a spectral resolution of 250,000. It covers the visible part of the spectrum and can be operated in intensity mode, to record Stokes-I line profiles of 2D images, and in polarization mode, to measure the full polarization state of the light along line profiles (I, Q, U, and V).

HELLRIDE (HELioseismic Large Region Interferometric Device) is a Fabry-Perot spectrometer that can scan 16 different solar lines, with 20 wavelength steps each, at a cadence of 60 seconds, in a field-of-view as large as 100100 arcsec2. This instrument is outstanding as it provides unique data to study atmospheric waves, and will help to understand how the chromosphere is heated by shock waves.

Instruments for SpectroscopyTeide Observatory, TenerifeVacuum Tower Telescope (VTT)Echelle spectrograph; a grating spectrograph with a predisperser, which allows to measure up to three different spectral bands at a spectral resolution of about 1 million. A reliable interaction with the telescope and the AO-Tip-Tilt system ensures that maps of solar regions-of-interest can be scanned.Data acquisition is performed with up to three of the following CCDs: PCO 1, PCO 2, & Sensicam (more details on CCDs below). On the slit (focal plane of telescope), the image scale is 4.49 arcsec/mm. The image scale in the focal pane of the spectrograph is 8.98 arcsec/mm.

TIP-II (Tenerife Infrared Polarimeter) is a near-infrared spectropolarimeter which is used together with the Echelle spectrograph to measure the Stokes profiles of near infrared spectral lines (1.0-1.8 m) with high spectral and spatial resolution. The solar surface can be scanned using a scanning unit

LARS (Absolute Reference Spectrograph) introduces a laser-frequency reference comb into the spectral images through a fibre optics system. Line positions can, consequently, be measured on an absolute wavelength scale.

Teide Observatory, TenerifeGREGOR (under preparing)

GREGOR is the new 1.5 m solar telescope currently assembled on Tenerife, Spain, by the German consortium of the Kiepenheuer-Institut fr Sonnenphysik, the Leibniz Institute for Astrophysics Potsdam, the Institut fr Astrophysik Gttingen, the Max-Planck-Institut fr Sonnensystemforschung and other international partners.Teide Observatory, TenerifeGREGOR (under preparing)The telescope is designed for high-precision measurements of the magnetic field and the gas motion in the solar photosphere and chromosphere with a resolution of 70 km on the Sun, and for high resolution stellar spectroscopy.The new Gregory type telescope with open telescope structure, alt-azimuth mount, complete retractable dome, adaptive optics and a pool of well established and new developed post focus instruments will replace the 45 cm Gregory Coud telescope at the Teide Observatory on Tenerife which will be retired after 40 years of service.

Teide Observatory, TenerifeGREGOR (under preparing)- 1500mm free aperture- Gregory configuration with additional tertiary mirror (M3)- light weighted optics- integrated adaptive optics- Image de-rotatornominal field of view 150" (max. 300")- effective focal length: 55.6m (F/38)- low instrumental polarisation- polarisation and calibration unit in symmetric beam- wavelength range from 350nm to several m- night time observations possible- mirrors made from silicon carbide (Cesic)- primary mirror (D=1,5m) active thermally controlled- M2 (D=0.43m) and M3 (D=0,36m) passive cooled

Teide Observatory, TenerifeGREGOR (under preparing)Hochauflsendes, zweidimensionales Spektro-Polarimeter2

Als eines der ersten wissenschaftlichen Instrumente wird ein Spektrometer mit zwei Fabry-Perot-Interferometern (FPI) im kollimierten Strahlengang zur Verfgung stehen. Fr Polarisationsmessungen kann ein Full-Stokes-Polarimter in den Strahlengang eingefgt werden.CCD Kameras mit 1376 x 1040 Pixeln aufgenommen. Bei der gewhlten Auflsung ergibt dies ein maximales Bildfeld von 52 Bogensekunden x 40 Bogensekunden. Die Kameras werden mit 12 Bit digitalisiert. Der spektraler Bereich reicht von 530 nm bis 960 nm, die spektrale Auflsung ist etwa 250 000.

524012530nm960 nm250 00010

Teide Observatory, TenerifeGREGOR (under preparing)Nacht-Spektrograph2Als eines der wenigen Sonnenteleskope kann GREGOR auch regelmig fr Nachtbeobachtungen eingesetzt werden. Dazu wird es mit einem fiberoptischen Doppelspektrographen ausgestattet. Die spektrale Auflsung betrgt etwa 100 000. Mit diesem Spektrographen sollen sonnenhnliche Sterne parallel im visuellen und blauem Spektralbereich beobachtet werden. Der Betrieb soll mglichst vollstndig robotisch erfolgen.

Teide Observatory, TenerifeGREGOR (under preparing)POLIS

Mit einem Nachbau des Polarimetric Littrow Spectrometer (POLIS) Instrumentes am VTT knnen gleichzeitige, polarimetrische Beobachtungen bei zwei bestimmten Wellenlngenbereich des sichtbaren und nahen ultravioletten Spektrums gemacht werden. Die spektrale Auflsung betrgt etwa 250 000. Die Installation des Instruments wird nach der Inbetriebnahme des Teleskops erfolgen.

Teide Observatory, TenerifeGREGOR (under preparing)Infrarot SpaltspektrographFr Beobachtungen im Wellenlngenbereich von etwa 1m bis 1.8m wird das GREGOR Teleskop mit einem Spaltspektrographen ausgestattet. Mit einer Kamera mit 1020 x 1024 Pixeln erhlt man ein Bildfeld von etwa 136 Bogensekunden x 137 Bogensekunden. Die spektrale Auflsung betrgt zwischen 380 000 bis etwa 570 000. Mit einem Polarimeter hinter dem Eintrittsspalt knnen die verschiedenen Polarisationszustnde des Sonnenlichtes gemessen werden.Fr die Zukunft ist geplant, den Spektrographen auch fr parallele Beobachtungen im optischen Wellenlngenbereich zu erweitern.

Roque de los Muchachos Observatory, La PalmaSwedish Solar Telescope (SST)TheSwedish 1-m Solar Telescope (SST) is a refractingsolar telescopeatRoque de los Muchachos Observatory,La Palmain theCanary Islands. It is run by theInstitute for Solar Physicsof theRoyal Swedish Academy of Sciences. The primary element is a singlefused silicalens, making it the secondlargest optical refracting telescopein use in the world. The 110-cm lens has aclear aperturediameter of 98cm. The SST is most often used as aSchupmann telescope, thereby correcting thechromatic aberrationsof the singlet primary.The SST is a vacuum telescope, meaning that it is evacuated internally to avoid disruption of the image from air inside. This is a particular problem with solar telescopes because of the heating from the large amounts of light collected being passed on to any air causing image degradation. As of 2005 it has produced the highest resolution images on the Sun of any telescope, using itsadaptive opticssystem.

Roque de los Muchachos Observatory, La PalmaSwedish Solar Telescope (SST)Currently, the SST is operating with anadaptive opticssystem with a 37-actuatordeformable mirrorfrom AOPTIX, although upgrades are underway.

Roque de los Muchachos Observatory, La PalmaSwedish Solar Telescope (SST)Details of the box holding the field mirror and field lens.B. The Schupman corrector with one lens and one mirror.C. The re-imaging optics, located on the optical table and consisting of a tip-tilt mirror, an adaptive mirror and a re-imaging lens.

Roque de los Muchachos Observatory, La PalmaSwedish Solar Telescope (SST)Instruments

The SST has two modes of operation.

One mode is a spectrograph mode, using the TRI-Port Polarimetric Echelle-Littrow(TRIPPEL) spectrograph with aresolutionof R = 230 000 (corresponding to 1.3km/s at the solar surface). TRIPPEL is aLittrow spectrographusing a 79 grooves/mmechelle gratingwith a blaze angle of 63.43 degrees.Roque de los Muchachos Observatory, La PalmaSwedish Solar Telescope (SST)Instruments

The other mode is an imaging mode, where imaging is split up in a red and a blue beam by a dichroic beamsplitter. The red beam has a tunable filter calledCRisp Imaging SpectroPolarimeter(CRISP) which operates from 510 to 860nm and is able to measure polarization by using liquid crystal modulation combined with a polarizing beamsplitter. The total system uses three 1k 1k Sarnoff CCDs, two are used for direct observations and the third is used in aiding theMOMFBDimage reconstruction method. The blue beam is a setup with a total of 4 MegaPlus II es4020 cameras.Big Bear Solar Observatory* Built by theCalifornia Institute of Technologyin 1969.* In 1997, transferred to theNew Jersey Institute of Technology(NJIT).* The surface of Big Bear Lake is about 2,055 meters (6,742ft) abovesea level.* The main observatory building is in the open waters of the lake.The originalmain solar telescopes:

a 65cm (26in) vacuum reflector

Its Main purpose was studies ofsunspots on the solar surface.

In early 2007, The New Solar Telescope (NST) was began building. - December 2008, first engineering light at the Nasmyth focus- January 2009, solar observations began. - The telescope is set on anequatorial mount. - 1.6m (63in) clear aperture open frame, off-axisGregorian telescope. - new ventilated dome

Big Bear Solar ObservatoryThe New Solar Telescope (NST)Big Bear Solar ObservatoryThe New Solar Telescope (NST)

In early 2007, The New Solar Telescope (NST) was began building. - December 2008, first engineering light at the Nasmyth focus- January 2009, solar observations began. - The telescope is set on anequatorial mount. - 1.6m (63in) clear aperture open frame, off-axisGregorian telescope. - new ventilated dome- f/2.4 primary mirror (M1)- 83.2m effective focal length (f/52 at Gregorian focus)- Telescope optics (PM,SM) made of Zerodur ().- Plate scale 2.48 arcsec/mm- Diffraction limited resolution of 0.06" at 500nm and 0.2" at 1,565nm (with AO)

- Computer controlled pointing and tracking- Real-time systems for maintaining telescope alignment- Temperature monitoring at many points on the telescope

- Active optics & Adaptive optics

- Gregory-Coud focus => 2 arcmin FOV Wavelength range from 0.39-1.6m with AO

- Nasmyth focus => All wavelengths > 0.39m also at with tip/tilt but without AOBig Bear Solar ObservatoryThe New Solar Telescope (NST)

Big Bear Solar ObservatoryThe New Solar Telescope (NST)Instruments for imagingBig Bear Solar ObservatoryThe New Solar Telescope (NST)4

BFIsVISIRIMNIRIS

Instruments for imagingBig Bear Solar ObservatoryThe New Solar Telescope (NST)

Instruments for imagingBig Bear Solar ObservatoryThe New Solar Telescope (NST)

Instruments for imagingBig Bear Solar ObservatoryThe New Solar Telescope (NST)

Instruments for imagingBig Bear Solar ObservatoryThe New Solar Telescope (NST)

IRIM

Instruments for SpectroscopyBig Bear Solar ObservatoryThe New Solar Telescope (NST)Fast Imaging Solar Spectrograph (FISS)collaborative work between Seoul National University (SNU) and Korean Astronomy and Space Science Institute (KASI)

Concept of two-mirrored field scanner.Instruments for Spectroscopy Big Bear Solar ObservatoryThe New Solar Telescope (NST)Fast Imaging Solar Spectrograph (FISS)

As of now, FISS is undergoing lab tests at KASI. Alignment test on a horizontal optical table was successful. The FWHM at the focal plane was 2.5 pixels and this can be regarded as moderate sampling. Still imaging test using coelostat is ongoing. Finally, it should undergo the same procedure on a vertical optical table, which is the same environment at the Coudlab of NST.Instruments for Spectroscopy Big Bear Solar ObservatoryThe New Solar Telescope (NST)

Hida ObservatoryDomeless Solar Telescope (DST)

1

PULNiX

CCD KODAK Mega-Plux4.2i

G

H

VMGCircamPCdstraidircam2PC

Ca II K (Morita et al. 2010)

() ()

sinsin(1)

/ / / cos (2)

/ /1.22 (3)1.221.22cos /cosABCND

632/mm6302.5

=54.29=51.38 (=2.907)

(1)m6302.525210(1)sinsin107/632(sin(54.29)+sin(51.38)25210(2)d/d = m / d cos = 4 /(107/632) cos(51.38) = 4.0510-4 [rad/] = 5.689 [mm/] N = (632/mm400 mm)(3)/ /1.22 632400 4 / 1.22 828852 828852 6302.5 828852 0.00760 1201/mm7773 =32.98=22.90 (=10.08 for port-6)1(1)m77737773(1)sinsin107/1201(sin(22.90)+sin(32.98) 7773(2)d/d = m / d cos = /(107/1201) cos(32.98) = 1.43210-4 [rad/] = 1.430 [mm/] = 0.699 [/mm]9.985mN = (1201/mm160 mmcos) (3)/ (1201160/cos(22.90)) 1 208601 208601 7773 208601 0.0372 6