Information For Observers

Index of this page

  1. About MagAO
  2. Instrument Parameters
  3. Observing at LCO
  4. Travel Logistics
  5. Resources

2015B Telescope Proposals

The 2015B run will probably be ~mid November — ~mid-late December 2015.  We offer these provisional dates for planning purposes only; we cannot guarantee the final dates at this time.

Proposals are due to Arizona TAC on Wednesday April 1st at noon MST (


New ADC info for fixed PA (non-ADI) VisAO observers

NOTE: This affects VisAO only. The ADC does not impact Clio observations.

The Atmospheric Dispersion Compensator (ADC) that feeds the PWFS and VisAO camera has one of its wheels (wheel 1) mechanically restricted to 0-180 degrees of rotation. This affects only the non-ADI mode of VisAO. If you need a fixed PA (in other words “observing with the rotator following”) for your VisAO observation — as long as you can have a 180 degree “flip” in your image PA (e.g. either a fixed PA=90 or 270 will work for the observation) there is likely no issue with the ADC fully operating for your observation.

However, for very rare observing conditions, the restricted ADC range might matter. The only case where this is likely to matter is if a PA is required for Clio observations (e.g. slit alignment) AND VisAO data are also desired. NOTE: If only Clio data are desired, then this issue does not affect your observations. We note that none of the VisAO programs executed in 2014B were affected by this issue.

However, if (for some rare reason) you have an absolute PA that must be exactly set for your VisAO observation (e.g. PA=90 is needed and PA=270 absolutely cannot work), then there is a ~50% chance that you will have to observe without ADC correction — depending on the exact time of the observation. None of the 2014B programs needed this rare mode. In fact, the ADC correction is working better than in previous runs thanks to new ADC “fine tuning” software from Jared Males and Alfio Puglisi. If you think your observations might be affected, please contact Jared Males.

About MagAO

MagAO is a facility instrument at a classically-scheduled telescope, which means that PIs are responsible for executing their own programs.  Because of the complexity of the AO system, we have MagAO team members available on-site and remotely who assist as much as we can.  To come prepared, please read the VisAO and/or Clio manuals, create your star catalog according to the LCO format, and be generally ready to take your data.  Please refer any questions about the details of this policy to Laird Close.

  • Other publications here.

Science cameras:

  • VisAO visible-light camera (600 – 1050 nm)
  • User’s manual
    • VisAO is a fast, low-noise visible CCD (the VisAO camera). The VisAO CCD is 1024×1024 E2V CCD47 which can be read at high speed if desired (details here (PDF documentation)). The platescale is 0.008″/pix. The VisAO camera has broadband r’, i’, z’, y filters and narrowband Hα, Hαcont, [SII], [SII]cont, [OI], and [OI]cont filters. It also has a r~0.1″ 0.001 transparent coronagraphic mask that may (must) be used with the broadband filters for deep bright star VisAO science. The PIs of VisAO are Laird Close (lclose at and Jared Males (jrmales at ) — please contact them if you have any questions about VisAO.
  • Clio2 near-IR camera (1 – 5.3 μm)
  • User’s Manual
    • Clio2 is a 512×1024 1-5.3 um imager with two cameras, either 15.85 or 27.49 mas pixels (Narrow camera FoV: 8×16”, Wide camera FoV: 14×28”). It has J, H, Ks, L’, M’, and 3.1, 3.3, 3.4, and 3.9 um filters available. There is also a low resolution (R~130 at 3.5 um; R~30 at K) prism-based spectrograph, not yet fully commissioned. Clio2 is currently sky-limited longwards of H, with readnoise of 70 e- that dominates at J and H, hence, J and H are offered as shared risk in 2014B. The Clio2 PI is Phil Hinz (phinz at ) please contact Phil or Katie Morzinski (ktmorz at for questions about Clio2.

Adaptive optics:

  • Wavefront sensor: Modulating Pyramid
    • 36-400 modes
    • 100-1000 Hz
  • Deformable Mirror: Adaptive-Secondary Mirror
    • 564 illuminated actuators
    • d = 23 cm
  • Control
    • Modal gain: tip/tilt, low-order, and high-order gain settings
    • Selectable subaperture size via CCD pixel binning

Instrument Parameters


On-axis:  Please allow ~15 minutes overhead for slewing, collimating, and setting up on a new target.  It is possible to acquire targets faster than this when the subsequent guide star is the same approximate brightness and location in the sky as the previous guide star (and if sky conditions haven’t changed), but 15 min. is a good rule of thumb.

Off-axis:  Please allow ~30 minutes overhead for set up on a new off-axis guide star target.


The J and H filters are readnoise, not sky, limited — due to the 70 electrons of read noise that the current (soon to be replaced) Clio2 detector suffers from. This not an issue at the longer wavelengths where Clio is optimized. Hence J and H are offered as shared-risk in 2014B.



AO system
Natural guide star (NGS) limiting magnitude I~14 (I~16 for Clio2 at K, L, M)
NGS angular resolution (λ/D at Pyramid, in good conditions) ~20 mas
NGS offset from science target up to 40” for Clio2, up to 8” for VisAO
AO performance – Bright NGS (R~8) Strehls: 30% i’ – 80% H (see plot below)
AO performance – Faint NGS (R~13) Strehls: 13% z’ - 40% H
Elevation lower limit (ASM safety) 30 degrees (airmass 2)
VisAO User’s manual
Diffraction limit 20 mas (r’) to 30 mas (z’)
Field of view and plate scale  8” x 8” FoV with 8 mas pixels (~Nyquist r’)
Filters (filter curves)
  • Broadband: r’ i’ z’ Ys
  • Full-FoV ND 3.22 selectable with r’,i’,z’, and Ys bandpasses
  • Narrowband: Hα Hαcont [OI] [OI]cont [SII] [SII]cont (note: FOV is 4″ X 8″)
Special features
  • pupil tracking
  • 0.1″ radius 0.1%-transparent (ND3) occulting spot
  • simultaneous spectral differential imaging (SSDI) in , [OI], and [SII] in PI-mode
  • high-speed readout
  • triplet ADC
  • Strehl-selection shutter (experimental)
Clio2 User’s Manual
Diffraction limit 38 mas (J) to 168 mas (M)
Field of view and plate scale
  • Narrow camera (f/37.7) — 16” x 8” FoV with 15.85 mas pixels (~Nyquist J)
  • Wide camera (f/21.5) — 28” x 14” FoV with 27.49 mas pixels (~Nyquist K)
Filters (filter curves)
  • Filter wheel 1:
    • 3.1um, 3.3um, L’, 3.9um, M’, prism, PK50 (blocks > 2um), open
      • (Old FW1: J, 3.1um, L’, M, M’, prism, open, blocked — used for Comm1 & 2, 2012B & 2013A)
  • Filter wheel 2:
    • J, H, Ks, Lspec (passes 2.8-4.2um), blocked, ND2 (4.4%), ND3 (0.1%), open
      • (Old FW2: H, Ks, 3.3um, 3.4um, 3.9um, ND2 (~1%), ND3 (0.1%), open — used for Comm1 & 2, 2012B & 2013A)
Special features
  • pupil tracking
  • pupil imaging mode
  • 3- and 6-hole non-redundant masks (NRM) — see Fig 1 in this post
  • apodized phase plate (APP) coronagraphs (to be commissioned) — see Fig 1 in this post
  • prism (R~130 at L and R~30 at K) (to be commissioned)
  • 3 slits: 0.06”, 0.12”, 0.36” width (to be commissioned)
Las Campanas Observatory 29.0° S, 70.7° W, 8000′ high
Telescope 6.5-m Magellan Clay
Seeing, 75th %ile 0.8”

Predicted Strehl Curves

Predicted Strehl

Predicted Strehl curves for various NGS magnitudes.  On-axis, low airmass, bright stars only. These curves do not accurately depict faint guide star performance.

Observing at Las Campanas Observatory

    • Prepare your starlist according to this catalog format; you will upload it to one of the computers in the control room where the telescope operator can access it.
    • Here is a little IDL program that will convert a space or comma separated file with the following columns into the proper Magellan catalog format: (1) target name, (2) RA, (3) Dec, (4) rotator mode and (5) comments
  • Specifying Guide Star Magnitude

    It is helpful if you have an accurate estimate of the magnitude of your guide star in the MagAO PyWFS bandpass. This is a critical parameter for optimizing the AO loop setup for your science, and being close will save time on sky. For most objects, standard I band will be the closest approximation. Note that we have found that SIMBAD reported magnitudes can be as much as ~1 magnitude bright, especially for redder stars. We find much better agreement using the USNO UCAC4 photometry [link to VizieR]. Another excellent resource is the DENIS survey I magnitude [link to VizieR].

    Here is what the MagAO WFS bandpass looks like:


    The MagAO Pyramid WFS bandpass.

    This plot gives some idea of how to transform magnitudes in V,R, and I to the WFS filter, based on spectral type.

    transform me

    MagAO PyWFS colors of main sequence stars. The points are based on closed loop on-sky results, using WFS reported magnitudes and USNO UCAC4 photometry. The curves are calculated using the Pickles spectral atlas.

    Wind Limits

    If a wind gust larger than the following values has been reported on the LCO Weather page in the last 15 minutes, the associated pointing limits apply. The wind direction will be based on the LCO weather page wind rose, and will be decided by the AO operator. In the case of shifting winds, it does not have to be a single value, but could be a range.

    • >= 20 mph : > 90 degrees from the wind direction
    • >= 30 mph: > 120 degrees from the wind direction, and below 80 degrees elevation.
    • >= 35 mph: dome closed


    Rotator Settings

    • Rotator angle is relative to the telescope axis. A position of 0 is aligned with the telescope.
    • To track, we recommend using one of these “on” rotator modes. Offsets can be made from an initial rotator position by request to the T.O. in any of these modes.
    • GRV – use this if you don’t care about PA, you just want it to be constant. This mode will maximize the amount of time the instrument is mostly vertical.
    • EQU – use this to set a specific PA on the detector.
    • To NOT track, we ask the T.O. to stop tracking — do not use the OFF setting in your catalog.

Travel Logistics

  • Travel Planning
    • Network Connection Request — Fill this out so you can use wi-fi and ethernet at the observatory (give several days advance notice).  You need your hardware MAC address for each connection you wish to make, i.e. both wi-fi and ethernet for all devices.  Note that if you have a new MacBook Pro, the MAC address is specific to the ethernet dongle (since it’s assigned to hardware), and you have to plug that in to even find the MAC address.  You want to have both wi-fi and ethernet enabled, because one or the other might work better in your dorm room, depending on which room you’re in.


  • What to Bring:
    • Only limited quick-look capabilities are available in the control room.  You will want to have your own laptop with a data-transfer capability (rsync, scp) and a FITS analysis capability (IRAF, IDL, Python, Matlab, whatever you prefer) so that you can monitor your data quality and make on-the-fly decisions as you take your data.
    • You must copy your data over to your own storage.  Bring a USB drive or harddrive with enough space.  Typical data quantities:
      • Clio: ~5-15 GB/night
      • VisAO: ~1-10 GB/night (up to 40 GB in extreme cases)
    • Flashlight/torch, coat, etc.
    • Other notes on physical comfort:
      • Dorm rooms have en-suite bathrooms.  Provided for you are sheets, blankets, pillows, towels, toilet paper, paper towels, and bars of soap.  LCO is dry, even to the Arizonans, so you may want to bring hand lotion and lip balm.
      • There is a clothes washer and dryer, with laundry detergent, under the stairs when you enter the lodge/diner.
      • If you want to get some exercise other than walking up and down the hill, you can run along the road which has both asphalt and gravel sections, or you can go to the (limited) gym.


  • Before You Go:
    • UPDATE 2015 January:No More Daylight Savings
    • Time changes: During an “A” semester (i.e. northern spring), it is sometimes necessary to set your phone or computer to Buenos Aries time upon arrival in Santiago, because the “Santiago” time your operating system picks will not know about the updated schedule for Daylight Savings time.
      • e.g. for 2014: Check here for google-translated information from Chile’s Department of Energy about the winter schedule. The Chilean Government has adjusted the daylight savings dates to conserve energy.  Winter starts midnight Saturday April 26th 2014, and ends midnight Saturday Sept 6th 2014.  (Hat-tip to J. M. Fernandez on Astronomers FB group.)
    • Please read the LCO Visiting Observer Guide.  Print it out and carry it with you when you travel, as it contains many useful phone numbers and other detailed information that you may need if your flight is delayed or there are other issues while traveling.
    • LCO Mountain Phone List — Note that “Sala de reuniones” is the Meeting Room in the ASB — it is a Vonage internet phone and the number is a California area code so you can call from the USA. There is also a Clay internet phone #. Note that these phones don’t work if the mountain internet connection is down, which happens on order of once per month (due to things like construction cutting a cable).
    • Please read the LCO Basic Safety Guide
    • NOTE: The Reciprocity Fee was discontinued in March 2014, reciprocally after the U.S. rescinded the Chilean Visa Fee.  We retain this paragraph so we can tell you it’s rescinded now, in case you hadn’t heard.  And the historical information:  Reciprocity fee — (NOTE: This is NOT official information!) — US citizens are required to pay a one-time reciprocity fee (kind of like a visa fee), upon first entry to Chile.  This is currently (2012) $160.  You get a stamp and receipt stapled into your passport, and it is good until your passport expires.  If you pay with cash you have to have perfect-looking US bills.  I recommend paying with credit card, so that you get a little credit-card slip you can use as a receipt to get reimbursed, because the real receipt is stapled into your passport.  (Although I heard it’s OK to remove the receipt after you return to the US from your first trip, it’s always iffy to have anything non-standard during border entry.)  Note that you have to go stand in an extra line to pay this fee, upon entry at Santiago and before you go through the regular Customs line, before you catch your flight to La Serena.  You also get an entry slip at the border that you need to show when you exit the country, so don’t lose that.


  • Other Info:
    • Power outlets — You will most likely be okay with your USAmerican power plug adaptors.  Up at the telescope control room there are plenty of US-based power attachments, and the dorm rooms given to observers are usually the ones with USAmerican power plugs too.
    • Food — LCO has an amazing team of chefs and the food is varied, delicious, and healthy.  This is at the dining hall down by the dorms.  Up at the telescopes or in the library/astronomer support building, there are little kitchenettes stocked with fruit, cheese & crackers, and cookies.  Note that during MagAO’s first commissioning run, we had at least a dozen team members in the control room, and it got quite crowded and supplies were running low… but we never ran out of cookies!
    • Meal times — Breakfast/Desayuno = 7:30-8am, Lunch/Almuerzo = 12:30-1pm, Dinner/Cena = 6:30-7pm
    • One shared wall in each dorm room is a bit thin, so please be quiet in the rooms.


  • Payment: Observers are required to pay all charges associated with their stay at LCO with credit card when departing the mountain.  This is all charges including but not limited to: room & board, transportation, and masks if any.


    • This is an excellent tool for making nicely visualized airmass charts, from the Isaac Newton Group of Telescopes.
      • Instructions:
        1. Enter observing date and observatory [Las Campanas Observatory (Chile)]
        2. Coordinates: Upload file or enter like:   (no spaces in object name)
          • [HD4375] 00 45 59.2 -16 39 09
        3. Click [Retrieve] and your airmass chart will load in a new tab
    • This is an excellent AO guide star tool from Keck.  It finds different options than clicking [query around] in Simbad, so try that too.
      • Instructions:
        1. At upper right: Enter your target name and resolve with Simbad, or enter RA & Dec.  Click [Load Target].
        2. At lower right: Digital Sky Survey image will appear.
        3. At lower left: List of possible guide stars will appear (from USNO catalog).  Length of list can be quite short, depending on number of possibilities found.  Look at last few columns for bright stars (Rmag) and nearby stars (Dist — in arcsec).  Find a good one and click on its RA or Dec.
        4. At lower right: A green box will appear showing where the star is on the DSS image (your target is at the center with a yellow N/E arrow coming out).  If you like the guide star, click [Add Guide Star].
        5. At upper left: Your target and the guide star will now appear in the Keck starlist format.  Keep adding guide stars as you like.  You can also keep adding new targets and their guide stars too.  When you are done, click [Download List] and now you have a starlist to edit to the LCO format!

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