Phase 1:
Application & Science Definition

To submit the science case for your proposal to the Liverpool Telescope, please read this page of guidelines and information. Note that the current PATT form does not have an option for IO:O, so this must be specified as "Other" and the name given.

Contents

When do I apply?

You must wait until your Telescope Allocation Group (TAG) issues a Call For Proposals (CFP) for the upcoming semester. The CFP gives all relevant details (application procedures, current telescope performance, instruments for use etc) and usually has a deadline of 4-6 weeks from date of issue.

The exact date of CFP issue and related deadlines varies slightly from year to year. You can keep up to date with current deadlines by visiting the Important Dates page, but in general:

  • For semester A (1st February - 31st July)
    • expect a CFP in September/October the previous year
  • For semester B (1st August - 31st January)
    • expect a CFP in February/March of the same year

How much time is available?

The time available comprises time allocated for the semester, minus any time pre-allocated for continuing programmes, and is listed in the call for proposals.

To which TAG do I propose?

This is determined by the affiliation of the Principal Investigator:

What kind of time should I apply for?

There are five types of observing time that can be applied for. These are FLEXIBLE, FIXED, MONITOR, INTERVAL and PHASED:

  • FLEXIBLE time, as the name implies, means that the observations can be carried out at any time during the semester when the conditions (see below) are appropriate. It is not possible to put any time constraint on when the observations will be done.
  • FIXED time means that the observations will only be carried out at a specified time, or not at all. This kind of time is suitable for occultations, or observations which must be simultaneous with a scheduled observation on some other facility. No more than 10% of time awarded by any panel may be FIXED time.
  • MONITOR time is time allocated where observations of an object are required at a regular interval.
  • INTERVAL time is where observations are taken as often as possible as long as the interval between observations is never less than that specified.
  • PHASED (previously "ephemeris") time allows you to make an observation of a target at a particular phase of its periodic cycle. An example might be that you want to observe an eclipsing binary during the eclipse, but you do not mind which orbit during the semester that observation is obtained.

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What observing conditions should I apply for?

In order to allow the telescope to be flexibly scheduled in an efficient manner, we need observers to decide and specify the seeing and photometric conditions appropriate to their proposal. The TAGs will then have to balance the requests to ensure that there is a reasonable balance of such conditions.

Sky brightness

We define two sky brightness levels, BRIGHT and DARK. Bright time is defined as any time that the moon is above the horizon, whatever the phase. Dark time is whenever the moon is below the horizon. Therefore 50% of the time is bright and 50% dark. There is no concept of grey time.

Seeing

Seeing is split into three bands:

  • GOOD: Seeing better than 0.8 arcsec.
  • AVERAGE: Seeing in the range 0.8-1.3 arcsec.
  • POOR: Seeing in the range 1.3-3.0 arcsec. No observations are made when seeing is worse than 3 arcsec.

Scheduling is performed on the most recently available estimate based on real-time reductions of recently taken images. The seeing value you set in the observing constraint is compared against the scheduler's prediction for the what image quality will be acheived in the r'-band taking into account the current airmass of your target. For example, if you request AVERAGE seeing conditions, the scheduler might attempt the observation at any airmass if the current seeing is very good, but if the seeing is only average it might reject your target when low on the horizon because it predicts the conditions will be poor there. Scheduling is always performed on an assumption of r'-band so you might expect for example, u-band images to show FWHM larger than the criterion set in the observing constraint. If you require 1arcsec u'-band imaging, you should probably apply for GOOD conditions, not AVERAGE.

Photometric conditions

You can request time allocation for Photometric and Non-Photometric conditions. If you are awarded Photometric time by the TAG panel, we will endeavour to observe your program in photometric conditions only. If you request Non-Photometric time, your observations can be scheduled for any time. Note that photometric standards are obtained automatically every night and are available to anyone. You do not need to apply for time to get these standards for yourself.

What instruments are available?

See the call for proposals for your TAG for details of what instruments are avaiable. For shared risk instruments (e.g. IO:THOR) you should contact LT Phase 1 Support to discuss feasibility and possible collaboration arrangements before applying to use those instruments as they are not full common-user instruments that are supported for general use.

Pointing and tracking

The current pointing performance of the LT is 10 arcsec rms. Maximum unguided exposures are 120 seconds; maximum guided exposures are 30 minutes.

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How do I calculate how much time I need?

Overheads

Use the instrument-specific exposure time calculator first to determine your exposure time (Te), then add the following overheads depending on the instrument you are using.

RATCam overheads

To the calculated exposure time (Te) the following overheads must be added:

  • Acquisition time Ta - time taken to slew the telescope on target. This is 60 seconds.
  • Autoguider acquisition - only if you nominate to use the autoguider. This is 45 seconds.
  • Filter change time Tf. This is 5 seconds.
  • Readout time Tr. This is 10 seconds.
Example
Suppose you have a programme where you have 20 objects which you wish to observe for 10 nights in a row, with an exposure time of 60 seconds, through three different filters. In this example, the observer has decided not to use the autoguider.
  • For one 60s exposure only (i.e. only one filter), the total time T1 is
     T1 = Ta + Tf + Te + Tr = 60 + 5 + 60 + 10 = 135 s
  • However for three exposures of the same object, where a different filter is used each time (nf = 3), the total time spent on the object Tobj is:
     Tobj = Ta + nf ( Tf + Te + Tr ) = 60 + 3 (5 + 60 + 10) = 285 s
    Note that the acquisition time is only applied once; no slewing is required after the 1st exposure because the telescope is already on target.
  • For twenty different objects (nobj=20) slewing between each object, per night for ten nights (nN=10), the total time Ttot is:
     Ttot = nN nobj Tobj = 10 x 20 x 285 = 57000 s = 15.83 hours

    As the unit of allocation is integer hours, you should therefore apply for 16 hours of time.

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RINGO2 overheads

For RINGO2 a simple 60 second slew overhead is all that is required. No filter changes are possible, and the readout speed is negligible.

FRODOSpec overheads

Overheads for compulsory and recommended FRODOspec actions are:

  • Acquisition time (slewing plus moving the target onto the fibre bundle): 4 minutes
  • Each readout time: 20 seconds
  • Grating change: 20 seconds
  • Xenon arc exposure (recommended for wavelength calibration): 60 seconds
  • Tungsten lamp exposure (recommended for fibre tracing): 60 seconds

RISE overheads

RISE is now a common-user instrument. To calculate exposure times, use the 2x2 binned option for RATCam on the exposure time calculator. Note that no filter-change or readout time overheads need be applied when applying for RISE time; a simple 60 second slew overhead is all that is required. No filter changes are possible, and the readout speed is negligible.

Overheads for Multi-instrument Groups

Overheads incurred while changing from one instrument to another are set at 60 seconds.

Minimum Usable Fraction

In addition to your total request, you need to specifiy a minimum usable fraction (MUF). This was introduced to help the LT technical team schedule observations effectively, e.g., to decide whether to finish the observations for one programme or to start a new programme that may not be completed. Proposers are asked to specify the MUF for their programme in the technical case of their phase 1 proposal. For example, the MUF can be used to specify that "any observations would be usable" (MUF=1%), or "a complete or nearly complete sample is essential to achieve the science goals" (MUF=90%). The TAC may revise the MUF of successful proposals if they feel this is appropriate.

Maximum Group Length & Subscription Factor

Groups with a length less than or equal to one hour can be scheduled without restriction. Group lengths which are longer than one hour may also be scheduled. However in order that such long groups will not interfere excessively with continuing monitor programmes undertaken by the telescope, the following rule will apply.

"Long" groups (i.e. groups of length greater than one hour) are permissible, provided that the subscription factor is less than 0.5. The subscription factor is equal to the mean length of individual long groups in hours, divided by the mean cadence in days, taken over the observing period for these groups.

Example 1:
For a series of 10 three-hour long groups taken at regular intervals over an observing period of 3 months:
  • mean length of the individual groups is 3 hours
  • mean cadence is approximately 9 days
Therefore the subscription factor is 3/9 = 0.33 and this series of long group observations is permissible.

Example 2:
The same series of three-hour groups taken over an observing period of one month:
  • mean length of the individual groups is 3 hours
  • mean cadence is 3 days
Therefore the subscription factor is 3/3 = 1.00 and this series of long group observations is NOT allowed.

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Other restrictions and guidance notes

We endeavour to obtain all the data requested for programmes allocated time by the TACs, however you must remember that on any given night, a dozen or more astronomers are effectively sharing the single telescope. Compromises may sometimes be necessary. The LT operations staff therefore reserve the right to remove from the scheduler database any observations which seriously interfere with other programmes. If you can anticipate any such problems, contact us in advance and address them specifically in your application technical case, you will greatly increase the chances that together we will be able to come up with an appropriate observing strategy.

  • Maximum Group Length The LT is intended to be flexible and responsive to changing conditions and priorities. We therefore normally impose a limit of one hour on any single observing group. For details of possible exceptions see above.
  • Avoid Bright Stars One common problem is grossly saturated stars causing image persistence in the CCD. All users are requested to check the field around their targets for bright stars which could disrupt other observers in this way. For short exposures, we recommend avoiding any stars brighter than 8th magnitude unless you are defocusing the telescope or using a very low throughput filter, e.g., u'.

What happens if my application is successful?

You will be required to enter the full specification of your observations. You can do this either at the start of the semester (and hence your observations are available for scheduling all semester), or for Target Of Opportunity Proposals, at any time during the semester once you have details of the target. Entering your full specification is known as the "Phase 2" part of the process, and details of how to go about it can be found on the Phase 2 page.

How do I get help?

Help for technical queries with the proposal process (running the exposure time calculator, the templates, email submission etc) is available from LT Phase 1 Support. You can also email more general queries about using the telescope, although we can not write your technical case for you!

Applying through PATT

The only method of applying is to use the LaTeX style file and template to prepare your application. These are similar to the current PATT 2 form but contain additional information necessary for robotic operation. If your proposal is successful you will have to do a Phase 2 data entry where you give full details of your observations.

Both the template and the style file can be obtained from the links below:

PATT Electronic Submission Procedure

The only method of submitting Liverpool Telescope proposals to PATT is via this system. To submit your proposal you must send a single email to the account patt@telescope.livjm.ac.uk . The email must be formatted as follows:

  • in the BODY of the email include the filled in LaTeX template
  • as an ATTACHMENT send the uncompressed POSTSCRIPT VERSION of the proposal (i.e. the output from dvips). This should include any embedded figures within it. DO NOT send the figures separately.

Proposals should be no more than one page for the scientific case, one for the technical justification and one for the figures and tables. An additional page will be accepted containing only a table of targets, if required. The justification of the sample selection should be made within the science case.

The proposal will be automatically checked for conformance to these criteria on submission, and you should receive an automated email reply either giving details of any problems with your submission or the PATT number assigned to your proposal within an hour of submission. If you have any problems, contact the LT Support (phase 1).

PATT Proposal Expiry Policy

Unless a proposal has been specifically allocated time in an upcoming semester, it will be expired at the end of the current one. Please note carefully that the ONLY proposals with allocated time are those listed on the PATT allocations web page. If your proposal is not listed here and has not been awarded time for future semesters, you need to submit a new Phase 1 form.

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Applications through CAT

Applicants for CAT time should refer to the procedures at and download the normal CAT form from the CAT pages at the IAC [English] [Espanol]

Applications through CCI

Applicants for CCI time should refer to the procedures at and download the normal CCI form from the CCI page at the IAC.

Applications to the internal JMU TAG

Policy for non-JMU PIs applying for JMU-allocated time on the Liverpool Telescope

The LT JMU TAG wishes to avoid the situation of front-PIs for non-JMU led proposals. Instead, some non-JMU-led time can be awarded. The PI of a proposal should have good knowledge of the proposal's main scientific area and required data reduction.

Non-JMU led proposals can be awarded time subject to the following rules:

  1. The PI has a strong connection with JMU (e.g. previously employed, established collaboration with JMU researcher).
  2. There is a co-I who is currently employed by JMU.
  3. A maximum of 25% of the JMU time (when there is oversubscription) shall be awarded to non-JMU led proposals.

It is expected that the JMU co-I, by agreeing to be on the proposal, supports (1) above and the co-I will be a coauthor of publication(s) resulting from LT data obtained.

Southampton and Frodospec: The contribution of the University of Southampton in the development of Frodospec is recognized as fullfilling the requirement of establishing a strong connection with JMU. Proposals to use Frodospec, led by a University of Southampton PI, will be accepted by the JMU TAG but are still subject to the 25% rule in (3) above. Collaboration with LJMU staff as Co-Is is encouraged, but not mandatory. This policy will be subject to review at the times of renewal of the STFC Operations Grant.

The deadline for applications will be notified to potential applicants by email. Applicants should use the PATT forms and mail completed applications, in the format described for PATT above, to jmu@telescope.livjm.ac.uk.

Proposals should be no more than one page for the scientific case, one for the technical justification and one for the figures and tables. An additional page will be accepted containing only a table of targets, if required. The justification of the sample selection should be made within the science case.

JMU Proposal Expiry Policy

Unless a proposal has been specifically allocated time in an upcoming semester, it will be expired at the end of the current one. Please note carefully that the ONLY proposals with allocated time are those listed on the JMU allocations web page. If your proposal is not listed here and has not been awarded time for future semesters, you need to submit a new Phase 1 form.

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Applications through OPTICON

Previously, users wishing to use the LT with OPTICON support applied first through PATT/CAT/CCI and were then awarded the support afterwards. From semester 2010B onwards, users apply through a common OPTICON TAC instead. See here for full details of the OPTICON Transnational Access programme.

Applications for observing are made via a web-based proposal tool based on the NORTHSTAR system once the call for proposals opens. As soon as the call opens a notice is posted on the OPTICON website at www.astro-opticon.org