%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % % GaPS proposal % % First revision: 2005.09.20_10:54:13 % Last revision: 2005.09.30_14:31:12 % % original TeX version by somebody % 2002 Dec 12: LaTeX conversion by Amy Mioduszewski % 2002 Dec 12: Minor format changes by Amy Mioduszewski and Greg Taylor % 2002 Dec 13: Fixes by Amy in response to Richard Porcas comments % 2002 Dec 18: More minor fixes by Amy in response to Patrick Charlot % 2002 Dec 31: More minor changes by Amy re: Mike Garret plus improved % underlining % 2003 Jan 18: More minor improvements to the underlining by Amy % 2003 Jul 21-22: Added student info, rapid response science by Jim U. % 2003 Aug 28: Some cleanup by Greg in response to Patrick Charlot % % This is the VLBI proposal cover sheet. It is highly recommended % that you make a copy of this before editing. % Lines beginning with ``%'' give instructions as to what to fill in % or replace on immediately following lines. % % COVER SHEET, FRONT SIDE % %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \documentclass[10pt]{article} \paperheight = 8.5truein \paperwidth = 11.0truein \def\unter#1{\hbox to #1{\hrulefill}} \def\YES {\bigotimes} \def\NO {\bigcirc} \def\yes {\bigotimes} \def\no {\bigcirc} \def\SOME {\circ} \def\arcmin{$^\prime$} \def\arcsec{$^{\prime\prime}$} \voffset=-1.3truein \hoffset=-0.8truein \textwidth = 8.0truein \textheight = 10.5truein \begin{document} \parindent 0pt \moveleft 0.75in \vbox{ \centerline{\bf % VLBA % Proposal for VLBA (and affiliates) PROPOSAL COVERSHEET} } \vskip -0.2in \moveright 5.2in \vbox{ \fbox{\rule[-0.75in]{0in}{0.2in} \begin{tabular}{p{1.5in}} \vskip 0.5in \vskip 0.2in rcvd: \\ \end{tabular} }} \vskip -0.75truein \moveleft 0.3in \vbox{ DEADLINES: 1st of Feb., June, Oct. } \bigskip \moveleft 0.7in \vbox{ {\bf (1)} Date Prepared: \vskip -11pt \moveleft -1.2in \vbox{ % If you want to add a manual date replace the \today (below) with a date. \today }} \medskip \moveleft 0.78in \vbox{ \begin{tabular}{p{1.4in}p{5.6in}} {\bf (2)} Title of Proposal:&\parskip -12pt %% enter first line of title on next line GaPS: Galactic Plane Survey --- search for more K-band calibrators \\&\parskip -12pt\hskip 0.05in %% enter second line of title on next line (if necessary) suitable for VLBA and VERA \\ \end{tabular} } %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % If any of the authors has moved or is a first time user, please add a sheet % at the end of the Scientific Justification with their full address including % electronic mail, fax and phone number. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \moveleft 0.75truein \vbox{ \begin{tabular}{|p{1.6truein}|p{1.8truein}|p{2.25truein}|p{0.28truein}|p{0.48truein}|p{0.48truein}|} \hline &&&\multicolumn{3}{c|}{\underbar{Students Only}} \\ {\bf (3)} AUTHORS&\hfil INSTITUTION\hfil&\hfil E-mail\hfil&G/U&\hfil For \hfil&\hfil Ph.D.\hfil\\ (Add * for new location)&&&&\hfil Thesis?\hfil&\hfil Year\hfil \\ \hline \parskip -12pt %% enter first author name on next blank line. If this is the author's first %% VLA or VLBA proposal, or the affiliation has changed since the last %% proposal, please put a * after the name. L. Petrov &\parskip -12pt %% enter first author institution on blank line below (abbreviate to less %% than 27 characters) NVI, Inc./NASA GSFC &\parskip -12pt %% enter first author e-mail on next line Leonid.Petrov@lpetrov.net &\parskip -12pt %% If first author is student, enter "G" for graduate student or "U" for %% undergraduate student on the next blank line. If first author %% isn't a student, leave blank. %% Students at institutions outside the U.S. may not have the same %% distinction between graduate and undergraduate studies that is followed %% in the U.S. In such cases, just enter "G". &\parskip -12pt %% If first author is a grad student, is this observation for his/her Ph.D. %% thesis? Enter "Yes" or "No". If first author is not a graduate %% student, leave blank. &\parskip -12pt %% If first author is a graduate student, enter the Ph.D. year, whether %% or not this observation is for the Ph.D. thesis. \\ \hline \parskip -12pt %% enter second author name on next blank line. If this is the author's first %% VLA or VLBA proposal, or the affiliation has changed since the last %% proposal, please put a * after the name. Y.Y. Kovalev &\parskip -12pt %% enter second author institution on blank line below (abbreviate to less %% than 27 characters) NRAO, GB &\parskip -12pt %% enter second author e-mail on next line ykovalev@nrao.edu &\parskip -12pt %% If second author is student, enter "G" for graduate student or "U" for %% undergraduate student. If second author isn't a student, leave blank. %% Students at institutions outside the U.S. may not have the same %% distinction between graduate and undergraduate studies that is followed %% in the U.S. In such cases, just enter "G". &\parskip -12pt %% If second author is a grad student, is this observation for his/her Ph.D. %% thesis? Enter "Yes" or "No". If second author is not a graduate %% student, leave blank. &\parskip -12pt %% If second author is a graduate student, enter the Ph.D. year, whether %% or not this observation is for the Ph.D. thesis. \\ \hline \parskip -12pt %% enter third author name on next blank line. If this is the author's first %% VLA or VLBA proposal, or the affiliation has changed since the last %% proposal, please put a * after the name. E. Fomalont &\parskip -12pt %% enter third author institution on blank line below (abbreviate to less %% than 27 characters) NRAO, CV &\parskip -12pt %% enter third author e-mail on next line efomalon@nrao.edu &\parskip -12pt %% If third author is student, enter "G" for graduate student or "U" for %% undergraduate student. If third author isn't a student, leave blank. %% Students at institutions outside the U.S. may not have the same %% distinction between graduate and undergraduate studies that is followed %% in the U.S. In such cases, just enter "G". &\parskip -12pt %% If third author is a grad student, is this observation for his/her Ph.D. %% thesis? Enter "Yes" or "No". If third author is not a graduate %% student, leave blank. &\parskip -12pt %% If third author is a graduate student, enter the Ph.D. year, whether %% or not this observation is for the Ph.D. thesis. \\ \hline \parskip -12pt %% enter fourth author name on next blank line. If this is the author's first %% VLA or VLBA proposal, or the affiliation has changed since the last %% proposal, please put a * after the name. D. Gordon &\parskip -12pt %% enter fourth author institution on blank line below (abbreviate to less %% than 27 characters) Raytheon/NASA GSFC &\parskip -12pt %% enter fourth author e-mail on next line dgg@leo.gsfc.nasa.gov &\parskip -12pt %% If fourth author is student, enter "G" for graduate student or "U" for %% undergraduate student. If fourth author isn't a student, leave blank. %% Students at institutions outside the U.S. may not have the same %% distinction between graduate and undergraduate studies that is followed %% in the U.S. In such cases, just enter "G". &\parskip -12pt %% If fourth author is a grad student, is this observation for his/her Ph.D. %% thesis? Enter "Yes" or "No". If fourth author is not a graduate %% student, leave blank. &\parskip -12pt %% If fourth author is a graduate student, enter the Ph.D. year, whether %% or not this observation is for the Ph.D. thesis. \\ \hline \parskip -12pt %% enter fifth author name on next blank line. If this is the author's first %% VLA or VLBA proposal, or the affiliation has changed since the last %% proposal, please put a * after the name. M. Honma &\parskip -12pt %% enter fifth author institution on blank line below (abreviate to less %% than 27 characters) NAO Japan &\parskip -12pt %% enter fifth author e-mail on next line honmamr@cc.nao.ac.jp &\parskip -12pt %% If fifth author is student, enter "G" for graduate student or "U" for %% undergraduate student. If fifth author isn't a student, leave blank. %% Students at institutions outside the U.S. may not have the same %% distinction between graduate and undergraduate studies that is followed %% in the U.S. In such cases, just enter "G". &\parskip -12pt %% If fifth author is a grad student, is this observation for his/her Ph.D. %% thesis? Enter "Yes" or "No". If fifth author is not a graduate %% student, leave blank. &\parskip -12pt %% If fifth author is a graduate student, enter the Ph.D. year, whether %% or not this observation is for the Ph.D. thesis. \\ \hline \parskip -12pt %% enter sixth author name on next blank line. If this is the author's first %% VLA or VLBA proposal, or the affiliation has changed since the last %% proposal, please put a * after the name. H. Kobayashi &\parskip -12pt %% enter sixth author institution on blank line below (abbreviate to less %% than 27 characters) NAO Japan &\parskip -12pt %% enter sixth author e-mail on next line hideyuki.kobayashi@nao.ac.jp &\parskip -12pt %% If sixth author is student, enter "G" for graduate student or "U" for %% undergraduate student. If sixth author isn't a student, leave blank. %% Students at institutions outside the U.S. may not have the same %% distinction between graduate and undergraduate studies that is followed %% in the U.S. In such cases, just enter "G". &\parskip -12pt %% If sixth author is a grad student, is this observation for his/her Ph.D. %% thesis? Enter "Yes" or "No". If sixth author is not a graduate %% student, leave blank. &\parskip -12pt %% If sixth author is a graduate student, enter the Ph.D. year, whether %% or not this observation is for the Ph.D. thesis. \\ \hline \parskip -12pt %% enter seventh author name on next blank line. If this is the author's first %% VLA or VLBA proposal, or the affiliation has changed since the last %% proposal, please put a * after the name. &\parskip -12pt %% enter seventh author institution on blank line below (abbreviate to less %% than 27 characters) &\parskip -12pt %% enter seventh author e-mail on next line &\parskip -12pt %% If seventh author is student, enter "G" for graduate student or "U" for %% undergraduate student. If seventh author isn't a student, leave blank. %% Students at institutions outside the U.S. may not have the same %% distinction between graduate and undergraduate studies that is followed %% in the U.S. In such cases, just enter "G". &\parskip -12pt %% If seventh author is a grad student, is this observation for his/her Ph.D. %% thesis? Enter "Yes" or "No". If seventh author is not a graduate %% student, leave blank. &\parskip -12pt %% If seventh author is a graduate student, enter the Ph.D. year, whether %% or not this observation is for the Ph.D. thesis. \\ \hline \end{tabular} } \medskip \moveleft 0.7in \vbox{ \begin{tabular}{p{3.0in}p{2.0in}p{1.5in}} {\bf (4)} Related previous or current VLBI proposal(s):&\parskip -12pt %% enter related VLBI proposal numbers on next line BB023, BF071, BP110, BP118, BK124, BR076, BL115, BL122 & %% If this is a resubmission of a proposal change \NO to \YES below $\NO$ Resubmission \\ \end{tabular} } \medskip \moveleft 0.7truein \vbox{ \begin{tabular}{p{1.25truein}p{2.20truein}p{0.9truein}p{2.9truein}} \multicolumn{2}{l}{{\bf (5)} Contact author for scheduling: %% enter contact author's name on next line Ed Fomalont } &\parskip -12pt {\bf (6)} Telephone:\ &\parskip -12pt %% enter contact author's telephone number on next line +1-434-296-0232 \\ \parskip -12pt \hskip 0.72in Address: &\parskip -12pt %% enter first line of contact author's address on next line NRAO, 520 Edgement Road, \parskip -12pt&\hskip 0.63in Fax: &\parskip -12pt %% enter contact author's Fax number on next line +1-434-296-0278 \\ \parskip -12pt &\parskip -12pt %% enter second line of contact author's address on next line Charlottesville, VA 22903--2475 \\ \parskip -12pt &\parskip -12pt %% enter third line of contact author's address on next line email: efomalon@nrao.edu &&\\ \parskip -12pt&\parskip -12pt %% enter fourth line of contact author's address on next line &&\\ \end{tabular} } \medskip \moveleft 0.7in \vbox{ \begin{tabular}{p{1.4truein}p{1.5truein}p{0.7truein}p{1.0truein}p{0.7truein}p{2.2truein}} {\bf (7)} Scientific Category: &\parskip -12pt %% on the next few lines find the category that applies to your %% project and replace ``\NO'' with ``\YES'' on that line $\YES$ astrometry \& geodesy& $\NO$ galactic& $\NO$ extragalactic& $\NO$ other:&\parskip -10pt %% if you replaced $\NO$ on the previous line (next to "other"), give a short %% description (a couple of words maximum) of the type of observation %% on the next line \\ \end{tabular} } \smallskip \moveleft 0.7truein \vbox{ \begin{tabular}{p{1.8truein}p{1.3truein}p{1.1truein}p{1.6truein}p{0.1truein}} %% The next few lines apply ONLY to VLBA proposals for Rapid Response Science. %% See http://www.vla.nrao.edu/astro/ under "Proposer Information and %% Documentation" to see if your proposal qualifies. Please note that %% VLBA Exploratory Proposals and Target of Opportunity Proposals must be %% submitted to a different e-mail address than the standard. %% Exploratory: exploresoc@nrao.edu %% Target of Opportunity: toosoc@nrao.edu \ \ \ \ \ Rapid Response Science: &\parskip -12pt %% on the next few lines find the category that applies to your %% project and replace ``NO'' with ``YES'' on that line $\NO$ Known Transient & $\NO$ Exploratory & $\NO$ Target of Opportunity &\parskip -10pt \\ \end{tabular} } \medskip \moveleft 0.7in \vbox{ \begin{tabular}{p{0.3truein}p{0.5truein}p{0.6truein}p{0.5truein}p{0.5truein}p{0.5truein}p{0.5truein}p{0.5truein}p{0.5truein}p{0.6truein}p{0.8truein}} \multicolumn{10}{l}{{\bf (8)} Wavelength(s) requested (those not available on the global network are indicated with a small circle):}\\ & % on the next few lines find the wavelengths being requested and % replace the ``NO'' or ``SOME'' with ``YES'' on that line $\NO$ 90cm& $\NO$ 50cm& $\NO$ 30cm& $\NO$ 21cm& $\NO$ 18cm& $\NO$ 13cm& $\NO$ 6cm& $\NO$ 5cm& $\NO$ 3.6cm& $\NO$ 3.6/13cm\\& $\NO$ 2cm & $\YES$ 1.3cm& $\NO$ 7mm& $\NO$ 3mm\\ &\multicolumn{4}{l}{ % if network standard setup is being used, replace the ``NO'' with ``YES'' % on the line below $\NO$ Global Network standard bands }& \multicolumn{6}{l}{ % if frequencies other than network standard setups are being requested, % replace the ``NO'' with ``YES'' on the line below, and % enter the band(s) requested on the following blank line $\NO$ Special frequencies: }\\ &&&&&&& \vskip -10pt \rule{2.8in}{0.5pt} \end{tabular} } \medskip \moveleft 0.7in \vbox{\vskip -12pt \begin{tabular}{p{0.3truein}p{6.7truein}} \multicolumn{2}{l}{{\bf (9)} Recording format: % For VLBA only: % If you are proposing to observe with the default continuum setup, change % NO to YES on the line below, and skip ahead to item 10 (search for '(10)') $\NO$ Default continuum setup (VLBA only), % Default setups depend on the correlator and band(s) being used and whether % polarization measurement is requested. For the VLBA correlator, the % default setup is is an aggregate bit rate of 128 Mbits/sec, with dual % polarization and four or eight channels and one or two bit quantization, % depending on band. % Skip this item if you have selected `default continuum setup' above. % indicate the recording format by replacing the NO with YES on one % of the lines below $\NO$ VLBA/MkIV, $\NO$ MkIII: Mode % If Mark III recording, enter the requested mode on the following % line. Include double speed if that is what you want. } \end{tabular} \vskip -10pt \hskip 5.80in \rule{1.in}{0.5pt} } \moveleft 0.7in \vbox{\vskip -12pt \begin{tabular}{p{0.3truein}p{6.7truein}} &\multicolumn{1}{l}{Bandwidth per BaseBand channel: % Skip this item if you have selected `default continuum setup' above. % Give bandwidth of BaseBand channel filters in MHz on the next blank line. % If more than one bandwidth is to be used, give number of channels at % each bandwidth 8 MHz } \end{tabular} \vskip -10pt \hskip 2.69in \rule{1.in}{0.5pt} } \moveleft 0.7in \vbox{ \begin{tabular}{p{0.3truein}p{1.2truein}p{0.26truein}p{0.1truein}p{0.2truein}p{1.0truein}p{0.2truein}p{2.1truein}} &Aggregate bit rate:&\parskip -12pt % Skip this item if you have selected `default continuum setup' above. % for MkIV or VLBA format observations, indicate the aggregate bit rate. % Note: 128 Mbits/sec is the maximum sustainable aggregate bit rate for % the VLBA. Requests to use higher bit rates on the VLBA should be % specifically discussed in the scientific justification. 256 Mbits/sec % is generally the maximum, but 512 Mbits/sec may be available under % very restrictive conditions (on the VLBA, this is a maximum of 5 hours % of recording in a period of 15-20 hours). % Enter the aggregate bit rate (sample rate times number of baseband channels % times bits per sample) on the line below. 256 \parskip -12pt &(\ &\parskip -12pt % Skip this item if you have selected `default continuum setup' above. % for MkIV or VLBA format observations, enter the number of baseband % channels on the following line 8 \parskip -12pt & BB channels at\ &\parskip -12pt % Skip this item if you have selected `default continuum setup' above. % for MkIv or VLBA format observations, enter the sample rate in % MSamples/sec (32, 16, 8, 4, 2, 1, .5) on the % following line 16 \parskip -12pt & MSamples/sec of % Skip this item if you have selected `default continuum setup' above. % for MkIV or VLBA format observations, indicate if one bit or two bit % sampling is requested by changing ``NO'' to ``YES'' on one of the next % two lines $\NO$ 1 bit, $\YES$ 2 bit )\hfil \end{tabular} \vskip -10pt \hskip 1.7in \rule{0.62in}{0.5pt} \hskip 0.08in \rule{0.50in}{0.5pt} \hskip 0.95in \rule{0.50in}{0.5pt} } \medskip \moveleft 0.7in \vbox{ \begin{tabular}{p{2.0truein}p{0.4truein}p{0.6truein}p{0.4truein}p{1.5truein}p{1.0truein}} \multicolumn{1}{l}{{\bf (10)} % If this proposal requests multiple epochs, change the ``NO'' to ``YES'' % on the line below $\NO$ Multi-epoch observation:}\ &\parskip -12pt % If multi-epoch, enter number of epochs requested with this proposal % on the line below \parskip -12pt & epochs of\ & \parskip -12pt % enter number of hours requested per epoch on the line below \parskip -12pt & hours each, separated by\ & \parskip -12pt % enter the separation between epochs on the next blank line below. Include % units - eg ``4 months'' or ``2 days'' \end{tabular} \vskip -10pt \hskip 2.2in \rule{0.50in}{0.5pt} \hskip 0.80in \rule{0.50in}{0.5pt} \hskip 1.70in \rule{1.00in}{0.5pt} } \medskip \moveleft 0.7in \vbox{ \begin{tabular}{|p{1.5truein}|p{3.7truein}|p{2.0truein}|} \hline {\bf (11)} Network&\hfil Requested antennas\hfil &\hfil Total time requested \\ \hline EVN \& MERLIN &\parskip -12pt % REQUESTED ANTENNAS % List antennas requested from the EVN on the next blank line. % Do NOT say "ALL" but specify using the 2-letter station % codes as given below. Consult the EVN STATUS TABLE at the % EVN User Guide at http://www.evlbi.org to find out which % telescopes are available at your requested frequency(ies): % Eb Jb Wb On Mc Nt Tr Ur Sh Cm Hh Yb Mh Wz Ar % If this is an EVN+MERLIN request, include MERLIN in the list. &\parskip -12pt % On the line below, list the total time requested of the EVN antennas \\ \hline VLBA&\parskip -12pt % List antennas requested from the VLBA on the next blank line % (ALL may be specified) ALL &\parskip -12pt % On the line below, list the total time requested of the VLBA antennas $ 3 \times 24 $ hours \\ \hline other NRAO&\parskip -12pt % On the next blank line, list other requested NRAO antennas % For example, VLA (specify Y1 or Y27) &\parskip -12pt % On the next blank line, list the total time per antenna requested on % other NRAO antennas \\ \hline \multicolumn{1}{|l|}{ % On the next blank line, enter the name of another participating network % (e.g. DSN, SHEVE) } &\parskip -12pt % On the next blank line, list the antennas requested from that network % or unaffiliated antennas &\parskip -12pt % On the next blank line, list the total time time per antenna requested of % these antennas \\ \hline Non-VLBI Instruments&\parskip -12pt % On the next blank line, list coordinated simultaneous or quasi-simultaneous % observations required on other instruments - especially VLA for % polarization calibration or pulsar phase determination. % VLA time for such purposes can be allocated on the basis of this proposal &\parskip -12pt % On the next blank line, list the total time requested of these instruments \\ \hline \end{tabular} } \medskip \moveleft 0.75truein \vbox{ \begin{tabular}{p{7.0truein}} {\bf (12)} ABSTRACT (Do not write outside this space. Please type)\\ \vskip 1.7in \hrule width 7.0in \\ Scheduler use only\\ \parskip -12pt (8/03)\\ \vskip -2.3in % give a short description (abstract) of 150 words or less of your % proposed observation and what you want to accomplish on the % following lines \hspace{1em} The success of VERA and VLBA phase-referencing projects at frequencies above 15~GHz critically depends on the availability of calibrators within a few degrees of the target source. In particular, the insufficient number of calibrators near the Galactic plane severely affects studies of weak galactic objects, since this limits the number of sources which can be imaged and positioned. \hspace{1em} In coordination with a current VERA fringe-search survey of 3000 objects near Galactic plane, $ |b| < 5^\circ$, and at the distance $ < 10^\circ$ from the Galactic center, we request three 24 hour sessions with the VLBA for follow-up observation of $\sim 500$ good candidates detected with VERA to determine their mas-accurate positions and radio structures. The VLBA observations will dramatically increase the number of calibrators at K-band near the Galactic plane, and be extremely valuable for VERA with a calibrator-target separation range of $0.3^\circ$ to $2.2^\circ$. Results will be available on-line within 20 days after completion of correlation. % END OF INPUT FOR SIDE 1 \end{tabular} } \clearpage % START PAGE 2 \moveleft 0.7truein \vbox{ \begin{tabular}{p{7truein}} \multicolumn{1}{l}{{\bf (13)} Observation type: % On the lines below, replace the ``NO'' with ``YES'' for all that apply $\YES$ Interferometry, $\NO$ Spectroscopy, $\NO$ Pulsar, $\NO$ Phase referencing } \end{tabular} } \medskip \moveleft 0.7truein \vbox{ \begin{tabular}{p{7truein}} \multicolumn{1}{l}{{\bf (14)} Proposal is % If the proposal is suitable for dynamic scheduling (that is, the % observer will supply an observe file in GST which will be executed % when the status of the array and weather is satisfactory, and the % observer may not be notified until after the observation has taken % place) change the ``NO'' to ``YES'' on the line below. Note that % EVN, Global and VLBA+Effelsberg proposals are NOT SUITABLE for % dynamic scheduling. $\YES$ Suitable % if the proposal is unsuitable for dynamic scheduling (perhaps needing % coordination with some other instrument or requiring a fixed date % of observation, change the ``NO'' to ``YES'' on the line below, and % if the reason is not one of the above, indicate what it is in the % body of the proposal. % $\NO$ Unsuitable for dynamic scheduling. } \end{tabular} } \medskip \moveleft 0.7truein \vbox{ \begin{tabular}{p{7truein}} \multicolumn{1}{l}{{\bf (15)} Polarization: % Indicate the polarization to be recorded by replacing the ``NO'' with % ``YES'' on one of the lines below. $\YES$ Single Polarization~~ $\NO$ Dual Circular Polarization }\\ \hskip 0.5in Global network standard for single polarization is LCP for all $\lambda$s except 13cm (RCP) and 3.6cm (RCP). \end{tabular} } \medskip \moveleft 0.7truein \vbox{ \begin{tabular}{p{7truein}} \multicolumn{1}{l}{{\bf (16)} Tape usage (Show $<$recording time$>$/$<$total time$>$): % If a recording duty cycle substantially less than 100 \% being proposed, % enter on the next blank line the percentage of time when recording is to % occur. Otherwise, leave blank. } \end{tabular} \vskip -10pt \hskip 3.65in \rule{0.50in}{0.5pt} } \medskip \moveleft 0.7truein \vbox{ \begin{tabular}{p{0.3truein}p{1.2truein}p{1.1truein}p{1.2truein}p{2.6truein}} \multicolumn{2}{l}{{\bf (17)} Assistance required:}\\ & Observation Setup:& % If assistance is needed for observation preparation and setup, replace % ``NO'' with ``YES'' on the appropriate line below % Note that observe file preparation for the VLBA is available only to % novice users from U.S. institutions. $\NO$ Consultation,& $\NO$ Extensive help,& $\NO$ Observe file preparation\\ &Postprocessing:& % If assistance is needed for postprocessing, replace % ``NO'' with ``YES'' on the appropriate line below % Note that the calibration service provided by NRAO for the VLBA is % presently only available for simple VLBA experiments. % All EVN and EVN/Global VLBI projects correlated at the EVN correlator at % JIVE, are automatically pipelined. The apriori calibration files and AIPS % Calibration tables are available at:www.evlbi.org/pipeline/user_expts.html % Images of target sources are produced on the PIs request. $\NO$ Consultation,& $\NO$ Extensive help,& $\NO$ Calibration service \end{tabular} } \medskip \moveleft 0.7truein \vbox{ \begin{tabular}{p{0.3truein}p{6.7truein}} \multicolumn{2}{l}{{\bf (18)} Processor:~ % Change ``NO'' to ``YES'' on the appropriate line below to specify the % desired correlator. $\YES$ Socorro, $\NO$ JIVE, $\NO$ Haystack, $\NO$ Bonn, $\NO$ Washington, $\NO$ Other % If ``Other'' is specified, please enter the correlator name on % the next line. } \end{tabular} \vskip -10pt \hskip 5.40in \rule{1.00in}{0.5pt} \\ \begin{tabular}{p{0.3truein}p{6.7truein}} &\multicolumn{1}{l}{Special processing: % If cross polarized correlation is needed, replace ``NO'' with % ``YES'' on the line below (and indicate dual polarization recording % on item 15 above (search on '(15)'). $\NO$ XPol, % If pulsar gating is required, replace ``NO'' with ``YES'' % on the line below $\NO$ Pulsar gate, % If processing at multiple field centers is required, replace ``NO'' with % ``YES'' on the line below $\NO$ Multiple Fields: % If ``YES'' was entered for multiple fields, enter number of correlation % passes on the line below. } \end{tabular} \vskip -10pt \hskip 4.45in \rule{0.50in}{0.5pt} } \moveleft 0.7truein \vbox{ \begin{tabular}{p{0.3truein}p{1.0truein}p{1.0truein}p{2.4truein}p{0.6truein}} &Averaging time:& \multicolumn{1}{l}{ % Enter averaging time in seconds on the next blank line. % Leave blank for the correlator default averaging time. 1 sec }\hskip 0.5in & Spectral channels per baseband channel:& \multicolumn{1}{l}{ % Enter the number of spectral channels per IF channel on the line below 64 } \end{tabular} \vskip -10pt \hskip 1.55in \rule{0.60in}{0.5pt} \hskip 2.8in \rule{0.60in}{0.5pt} } \moveleft 0.7truein \vbox{ \begin{tabular}{p{0.3truein}p{6.7truein}} &\multicolumn{1}{l}{ % if other special processing is required, replace ``NO'' with ``YES'' % on the line below $\NO$ Other special processing: % if other spectral processing is required, enter a descriptive word on % the next line } \end{tabular} \vskip -10pt \hskip 2.3in \rule{3.60in}{0.5pt} } \medskip \moveleft 0.7truein \vbox{ \begin{tabular}{p{7truein}} \multicolumn{1}{l}{{\bf (19)} Postprocessing Location: % Enter the location where postprocessing is to be done on the line below % (e.g., NRAO-SOC, JIVE) NRAO-CV, NRAO-GB, GSFC } \end{tabular} \vskip -10pt \hskip 1.95in \rule{1.9in}{0.5pt} } \medskip \moveleft 0.7truein \vbox{ \begin{tabular}{p{0.3truein}p{6.7truein}} \multicolumn{2}{l}{{\bf (20)} Source list:\ \ % Change the ``NO'' to ``YES'' on one of the lines below, depending on % the equinox of the positions in the source list to follow: % Note - J2000 positions are preferred. $\YES$ J2000 $\NO$ B1950 }\\ &If more than 4 sources, please attach list. If more than 30, give only selection criteria and GST range(s) \end{tabular}} \medskip \moveleft 0.7truein \vbox{ \begin{tabular}{|p{1.85truein}|p{1.2truein}|p{1.2truein}|p{1.2truein}|p{1.2truein}|} \hline &\hfil Source 1 \hfil & \hfil Source 2 \hfil &\hfil Source 3 \hfil &\hfil Source 4 \hfil \\ \hline Name(s) &\parskip -12pt % On the following blank line, enter the name of the first source ALL SKY &\parskip -12pt % On the following blank line, enter the name of the second source &\parskip -12pt % On the following blank line, enter the name of the third source &\parskip -12pt % On the following blank line, enter the name of the fourth source \\ \hline RA (hh mm)&\parskip -12pt % on the following blank line, enter the right ascension of the first source 0--24h &\parskip -12pt % on the following blank line, enter the right ascension of the second source &\parskip -12pt % on the following blank line, enter the right ascension of the third source &\parskip -12pt % on the following blank line, enter the right ascension of the fourth source \\ \hline Dec (dd.d)&\parskip -12pt % on the following blank line, enter the declination of the first source --40d to +70d &\parskip -12pt % on the following blank line, enter the declination of the second source &\parskip -12pt % on the following blank line, enter the declination of the third source &\parskip -12pt % on the following blank line, enter the declination of the fourth source \\ \hline GST range (Europe)&\parskip -12pt % on the following blank line, requested European GST range, 1st source &\parskip -12pt % on the following blank line, requested European GST range, 2st source &\parskip -12pt % on the following blank line, requested European GST range, 3st source &\parskip -12pt % on the following blank line, requested European GST range, 4st source \\ \hline GST range (US)&\parskip -12pt % on the following blank line, requested US GST range, 1st source 0--24h &\parskip -12pt % on the following blank line, requested US GST range, 2st source &\parskip -12pt % on the following blank line, requested US GST range, 3st source &\parskip -12pt % on the following blank line, requested US GST range, 4st source \\ \hline GST range (Other) &\parskip -12pt % on the following blank line, requested GST range, 1st source, other antennas &\parskip -12pt % on the following blank line, requested GST range, 2st source, other antennas &\parskip -12pt % on the following blank line, requested GST range, 3st source, other antennas &\parskip -12pt % on the following blank line, requested GST range, 4st source, other antennas \\ \hline Band(s) &\parskip -12pt % on the following blank line, enter the band(s) at which the first source % is to be observed K &\parskip -12pt % on the following blank line, enter the band(s) at which the second source % is to be observed &\parskip -12pt % on the following blank line, enter the band(s) at which the third source % is to be observed &\parskip -12pt % on the following blank line, enter the band(s) at which the fourth source % is to be observed \\ \hline Flux density (Total, Jy) &\parskip -12pt % on the following blank line, enter total flux density of the first source $>$80 mJy &\parskip -12pt % on the following blank line, enter total flux density of the second source &\parskip -12pt % on the following blank line, enter total flux density of the third source &\parskip -12pt % on the following blank line, enter total flux density of the fourth source \\ \hline Flux density (correlated, mJy) &\parskip -12pt % on the next blank line, enter expected correlated flux density of the % first source $>$50 mJy &\parskip -12pt % on the next blank line, enter expected correlated flux density of the % second source &\parskip -12pt % on the next blank line, enter expected correlated flux density of the % third source &\parskip -12pt % on the next blank line, enter expected correlated flux density of the % fourth source \\ \hline RMS needed (mJy/beam) &\parskip -12pt % on the following blank line, enter needed RMS (mJy/beam), 1st source 3--5 mJy &\parskip -12pt % on the following blank line, enter needed RMS (mJy/beam), 2nd source &\parskip -12pt % on the following blank line, enter needed RMS (mJy/beam), 3rd source &\parskip -12pt % on the following blank line, enter needed RMS (mJy/beam), 4th source \\ \hline Peak/RMS needed &\parskip -12pt % on the following blank line, enter needed Peak/RMS needed, 1st source $>$30:1 &\parskip -12pt % on the following blank line, enter needed Peak/RMS needed, 2nd source &\parskip -12pt % on the following blank line, enter needed Peak/RMS needed, 3rd source &\parskip -12pt % on the following blank line, enter needed Peak/RMS needed, 4th source \\ \hline \end{tabular}} \smallskip \moveleft 0.75truein \vbox{ \begin{tabular}{p{7.0truein}} % At this point, if you are giving selection criteria instead of a % source list, you may insert a three line summary of the criteria. \parskip -12pt \\ \end{tabular}} \medskip \moveleft 0.75truein \vbox{ \begin{tabular}{p{0.3truein}p{6.7truein}} \multicolumn{2}{l}{{\bf (21)} Preferred VLBI session or range of dates for scheduling, and why:}\\ &\parskip -12pt % On the following line, enter preferred date or session Three sessions, each must be 24 hours in length. Winter preferred for phase stability. After Jan 1, 2006 when VERA reductions will be finished. \parskip -12pt \\ \end{tabular}} \medskip \moveleft 0.75truein \vbox{ \begin{tabular}{p{0.3truein}p{6.7truein}} \multicolumn{2}{l}{{\bf (22)} Dates which are NOT acceptable, and why: }\\ &\parskip -12pt % On the following line, enter dates which are not acceptable \parskip -12pt \\ \end{tabular}} % END OF INPUT FOR VLBI COVERSHEET, SIDE 2. \medskip \moveleft 0.75truein \vbox{ \begin{tabular}{p{0.3truein}p{6.7truein}} \multicolumn{2}{l}{{\bf (23)} Attach a self-contained scientific justification, not in excess of 1000 words.}\\ &Preprints or reprints will not be forwarded to the referees. \end{tabular}} \vskip 0.75in \moveleft 0.65truein \vbox{ \begin{tabular}{p{6.9truein}} Information about the capabilities of the VLBA may be found on the World Wide Web by starting at the NRAO home page, http://www.nrao.edu, and selecting the VLBA from ``Sites and Telescopes.'' \\ \\ A brief summary of the capabilities of the EVN antennas is given in the EVN STATUS TABLE in the EVN USER GUIDE, which may be found at http://www.evlbi.org/user\_guide/user\_guide.html. \\ \\ Please include the full postal addresses for first-time users or for those that have moved (if not contact author). \end{tabular}} \clearpage \textheight 9.3in \hsize=7in \columnwidth=7in %\pagestyle{plain} \voffset=-0.7in \hoffset=-1.3in \vsize=8.9in \parindent 20pt \normalsize %% TYPE YOUR SCIENTIFIC JUSTIFICATION BEGINNING ON THE NEXT LINE. %% DO NOT EXCEED 1000 WORDS. EXCESS TEXT MAY CAUSE YOUR PROPOSAL %% TO BE DOWNGRADED. % \end{document} {\large\bf\noindent GaPS: Galactic Plane Survey --- search for more K-band calibrators suitable for the VLBA and VERA} \section{Summary} We request three 24 hour sessions with the VLBA for observing 500 candidates in order to dramatically increase the number of calibrators at K-band near the Galactic plane for supporting VERA and VLBA experiments focused on the study of galactic objects. Previous observations with the VLBA in 1994--2005 in S/X produced a list of 2834 sources, with position accuracy better than 5 mas and with S/X images. However, the density of this catalogue is not sufficient to provide enough calibrators closer than $4^\circ$ near the Galactic plane for VERA and VLBA observations of many interesting galactic objects. VERA observations, in particular, critically depends on availability of calibrators within $2^\circ\hspace{-0.2em}.2$ of a target source. In October-November 2005, VERA is observing a list of 3000 potential candidates for fringe searching at K-band. Any source with a detectable fringes will then be followed up by the proposed VLBA observations. \section{Previous Observations} VLBA calibrator surveys, BB024, BF071, BP110, BP118 and BK124, were designed to expand the list of calibrator sources suitable for phase referencing and as target for geodetic observations. Twenty one VLBA Calibrator observing sessions, each of 24 hours, were made between 1994 and 2005. Each source was observed 2--3 times at different hour angles for 1.5--5 minutes. In this way up to 200 sources could be observed in each 24 hour session with sufficient sensitivity and $u$-$v$ coverage to determine their suitability as phase-reference calibrators. Analysis of these observations produced images and milli-arcsecond accurate positions of observed sources. The results from the above observations were published (Beasley et~al, 2002; Fomalont et~al, 2003, Petrov et~al, 2005a, Petrov et~al, 2005b, Kovalev et~al, in preparation) and were made available on the Web at \par\noindent {\tt http://www.vlba.nrao.edu/astro/calib/} and {\tt http://gemini.gsfc.nasa.gov/vcs/}. In the web sites, all sources within a specified distance from a selected target position can be found, images, $u$--$v$ plots and coordinates for each potential calibrator can be scrutinized. However, only 177 S/X calibrators are known near the galactic plane, and many may not be suitable as K-band calibrators. Thus, there is a dearth of good calibrations near the galactic plane. A small subset of VCS sources, 374 objects, was re-observed at K-band in 2002--2004 for future support of space navigation, proposals BR076, BL115, BL122, Jacobs et~al, 2003. Among 252 detected objects, 14 are are within $|b| < 5^\circ$. These observations showed that a) a majority of bright S/X calibrators were detected at K-band; b) the difference in position from K-band observations and X-band observations did not exceed 1~mas; c) the effect of ionosphere at K-band did not significantly degrade estimates of positions. \section{Impact of expected results} The dual-beam, four station radio interferometer VERA is designed for direct measurements of the parallax of hundreds of radio sources, such as H${}_2$O, SiO masers and late type stars, perhaps with accuracy as good as 10$~\mu$as. These measurements involve simultaneous observations of a pair calibrator-target separated within $0^\circ\hspace{-0.2em}.3$--$2^\circ\hspace{-0.2em}.2$ and recorded with independent receivers at K or Q bands. One of the primary goals of VERA mission is to improve the accuracy of the scale of distances used in astronomy, since at the 10$~\mu$as precision level trigonometric parallax of almost any object in the Galaxy can be directly determined. This scale of distances has a fundamental importance for various astrophysical applications. VLBA phase-referencing observations at high frequency of galactic objects is also a significant part of its proposal load. Often, the limitation above 15~GHz for image quality and positional accuracy is caused by the loss of coherence in the image because of the relative large distance of the calibrator from the target. Thus, the new list of calibrators in the Galactic plane will significantly expand the list of VERA target sources and will improve the phase-referencing VLBA projects studying weak galactic objects. \section{Proposed VLBA and VERA Observations} Because the area near the galactic plane is not well surveyed, the list of suitable candidates for VLBI calibrators is difficult to compile. First, a list of 3000 sources will be selected from several catalogs (NVSS, CLASS, etc.) utilizing the CATS database capabilities (Verkhodanov, et al., 1997) and using a rigorous procedure based on evaluation of a~priori probability of detection developed by Petrov et~al., 2005b. Applying this procedure in BP118 observing campaign resulted in an impressive detection rate of 65\% in the zones where no compact sources were previously found. Second, all 3000 of the sources will be observed by VERA in October-November 2005 in one scan each for 2~minutes at K-band recorded with 240~MHz bandwidth. Third, those sources for which fringes are detected, will be on the list for the VLBA observations we propose here. We estimate that up to 500 sources will be detected by the VERA observations. This estimate is based on extrapolating the number of sources in the VCS sample, which is complete at the 200~mJy level of the correlated flux density, to 60~mJy, the detection limit of VERA fringe searching observations. VERA system does not have capabilities to provide good maps and determine absolute position of sources with 1-mas accuracy which is required for support of dual-beam observations for measurements of parallaxes of galactic objects with 10$\mu$as accuracy. Thus, the VERA fringe searching survey is designed only to detect sources at K-band. But VERA has the sensitivity comparable to the VLBA, and the pre-selection of sources will significantly increase the yield of VLBA observations. We, thus, request three 24 hour observing sessions with the VLBA to observe about 500 candidates sources from the VERA fringe-search in the zone $ \delta > -40^\circ, |b| < 5^\circ $ as well as within $10^\circ$ from the Galactic center. We will use eight IF channels, spanned over 500~MHz around 24~GHz, with a total bandwidth of 64~MHz at 2~bit sampling, 256~Mb/s in order to reach the maximal sensitivity to reach the approximate VERA sensitivity. We request the same correlator setup as in the BP110, BP118 and BK124 proposals: 64~spectral channels in each IF and integration time 1~sec. This will give us an extra-wide search window needed for fringing sources with poorly known a~priori positions. The calibration and imaging will be made in Charlottesville and Green Bank by using standard packages AIPS and difmap. Positions will be determined with Calc/Solve at GSFC. The observation plan will be similar to the previous VCS schemes. Each source will be observed in two scans in different hour angles for 150 seconds. Every 1.5~hours, three to four troposphere calibrators will be observed. These calibrators are selected from the list of sources from the 2~cm VLBA survey (Kovalev et~al., 2005), which are brighter than 0.5~Jy and have compactness index greater than 0.5 at 15~GHz. During a burst of tropospheric calibrator observations, the sources are selected in such a way that each antenna would observe at least one source at elevation below $20^\circ$ and at least one source at elevation $50^\circ$ above the horizon. Results of the VLBA Calibrator survey showed that observing tropospheric calibrators and estimation of troposphere path delay in zenith direction together with other parameters reduces the contribution of the unaccounted tropospheric path delay to less than 0.5~mas. \begin{thebibliography}{9} \parbox{0.96\columnwidth}{ \bibitem{r1} Beasley,~A. J., in {\em Very Long Baseline Interferometry and the VLBA}, 1995 ASPCS, 82, 327 \par\vspace{-1.5ex}\par\noindent \bibitem{r2} Beasley,~A.~J., Gordon,~D., Peck,~A.~B., Petrov,~L., MacMillan,~D.~S., Fomalont,~E.~B., \& Ma,~C. 2002, ApJS, 141, 13 \par\vspace{-1.5ex}\par\noindent \bibitem{nvss} Condon, J.J., Cotton, W.D., Greisen, E.W., Yin, Q.F., Perley, R.A., Taylor, G.B., Broderick, J.J. 1998, AJ, 115, 1693 \par\vspace{-1.5ex}\par\noindent \bibitem{r4} Fomalont, E.~B., Petrov, L., MacMillan, D.~S., Gordon, D., \& Ma, C., 2003, AJ, 126 (N5), 2562. \par\vspace{-1.5ex}\par\noindent \bibitem{r5} Jacobs, C.~S., Charlot, P., Gordon, D., Lanyi, G.~E., Ma, C., Naudet, C.~J., Sovers, O.~J., Zhang, L.~D., Proc. \\ 25th IAU meeting, Sydney, 2003. \par\vspace{-1.5ex}\par\noindent \bibitem{r6} % Sub-milliarcsecond Imaging of Quasars and Active Galactic Nuclei. % IV. Fine Scale Structure Kovalev, Y.~Y., et al.\ %Kellermann, K.~I., Lister, M.~L., %Homan, D.~C., Vermeulen, R.~C., Cohen, M.~H., Ros, E., %Kadler, M., Lobanov, A.~P., Zensus, J.~A., %Kardashev, N.~S., Gurvits, L.~I., Aller, M.~F., \& Aller, H.~D.\ 2005, AJ, 130, in press (astro-ph/0505536) \par\vspace{-1.5ex}\par\noindent \bibitem{r7} Petrov, L., Kovalev, Y.Y., Fomalont, E.~B., \& Gordon, D., 2005a, AJ, 129, 1163. \par\vspace{-1.5ex}\par\noindent \bibitem{r8} Petrov, L., Kovalev, Y.Y., Fomalont, E.~B., \& Gordon, D., 2005b, AJ, Submitted, astro-ph/0508506. \par\vspace{-1.5ex}\par\noindent % CATS database \bibitem{cats} Verkhodanov, O.~V., Trushkin, S.~A., Andernach, H., \& Chernenkov, V.~N.\ 1997, in ASP Conf.\ Ser.\ 125, \\ Astronomical Data Analysis Software and Systems VI, ed.\ G.~Hunt, \& H.~E.\ Payne (San Francisco: ASP), 322 } \end{thebibliography} \end{document}