%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % % NPCS proposal % % First revision: 2005.09.28_12:18:40 % Last revision: 2005.10.02 % % 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 improvments 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} \usepackage{natbib} %\renewcommand{\baselinestretch}{0.99} \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 % Settings for natbib (yyk) \setlength{\bibsep}{0pt} \def\bibfont{\small} \renewcommand\bibsection{\subsection*{\refname}} \renewcommand\bibnumfmt[1]{} \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 Northern Polar Cap VLBA Survey \\&\parskip -12pt\hskip 0.05in %% enter second line of title on next line (if necessary) \\ \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. Y.Y. Kovalev &\parskip -12pt %% enter first author institution on blank line below (abbreviate to less %% than 27 characters) NRAO, GB &\parskip -12pt %% enter first author e-mail on next line ykovalev@nrao.edu &\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. L. Petrov &\parskip -12pt %% enter second author institution on blank line below (abbreviate to less %% than 27 characters) NVI, Inc./NASA GSFC &\parskip -12pt %% enter second author e-mail on next line Leonid.Petrov@lpetrov.net &\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. B. 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. &\parskip -12pt %% enter fifth author institution on blank line below (abreviate to less %% than 27 characters) &\parskip -12pt %% enter fifth author e-mail on next line &\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. &\parskip -12pt %% enter sixth author institution on blank line below (abbreviate to less %% than 27 characters) &\parskip -12pt %% enter sixth author e-mail on next line &\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 & %% 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 Edgemont 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 $\NO$ astrometry \& geodesy& $\NO$ galactic& $\YES$ 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& $\YES$ 3.6/13cm\\& $\NO$ 2cm & $\NO$ 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)') $\YES$ 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 } \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. \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 \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 \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, $\NO$ 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 We request three 24 hour sessions with the VLBA for S/X observing {\it a complete sample} of 500 sources in the zone with $\delta > +75^\circ $ with flux density $> 200$~mJy at 1.4~GHz regardless their spectral index value. Almost all previous VLBI surveys selectively observed flat spectrum sources and this limits the statistical studies to the classes of sources with relatively dominant cores. We expect to detect compact steep spectrum sources, FR\,I and FR\,II sources with radio cores, as well as core-dominated sources. With S/X observations, we will also obtain spectral information of the structure. The statistical studies will determine an unbiased estimate of the role of compact emission in all sources. The VLBA data will be supplemented by total instantaneous 2--22~GHz broad-band spectra measured at RATAN--600 in 2005. This will allow direct comparison of the parsec scale structure and compactness versus the continuum spectra. % 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. $\NO$ 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 +75d to +90d &\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 S/X &\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 $>$40 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 $>$20 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 $>$100:1 &\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 24 hour sessions. \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} \centerline{\LARGE\bf Northern Polar Cap VLBA Survey} \section{Summary} The focus of this proposal is to make a statistical study of the compact emission of {\it all} sources down to a relatively low level of flux density. All previous large VLBI surveys selectively observed flat spectrum sources that are nearly all core-dominated. We expect to image an unbiased sample of compact steep spectrum sources (CSS) and extended FR\,I and FR\,II sources with radio core. In order to achieve the proper sample for study, we request three 24 hour sessions for observing with the VLBA at S/X bands of {\it a complete sample} of 500 sources in the zone $ \delta > +75^\circ $ with NVSS flux density $> 200$~mJy at 1.4~GHz {\it regardless their spectral indexes}. The VLBA results will be supplemented by instantaneous broad-band spectra measured in 2005 at RATAN--600 in the 2--22 GHz frequency range including S and X bands. This will allow direct comparison of the parsec scale structure and compactness versus the total flux density continuum spectra. We will propose VLBA follow-up observations for identified CSS at a later date in order to produce and analyze higher dynamic range mas-scale images than the once resulting from this search experiment. \section{Previous Observations} From the previous 1994--2005 VLBA observations in the framework of the VLBA Calibrator survey (projects BB\,023, BF\,071, BP\,110, BP\,118, BK\,124) and 53~RDV observing sessions, positions of 3331 sources were determined and images of more than 2400 objects were produced (Beasley et~al.~2002; Fomalont et~al.~2003, Petrov et~al.~2005a, Petrov et~al.~2005b, Kovalev et~al, in preparation). Among them, a subset of $\sim$2000 objects with $ \delta > -30^\circ $ forms a homogeneous, reasonably complete ($>$95\%) sample of flat-spectrum sources with correlated flux density greater than 200~mJy at 8~GHz. Completeness of the sample and uniformity of the data reduction permits robust statistical analysis of this population of bright compact flat spectrum sources, such as: population modeling of the observed core brightness temperature in order to estimate distributions of the intrinsic core brightness temperature, the viewing angle, and Doppler brightening; expanding the cosmological significance of core-jet angular size versus redshift distribution, comparing the compactness of radio structures with IDV properties; correlating the radio core properties with optical class; etc. However, the selection of candidates for the VLBA Calibrator surveys and the RDV programs was focused on observing the sources with a spectrum flatter than $-0.5$ ($S\sim\nu^{+\alpha}$), which comprise approximately 15\% of the entire population of radio sources at centimeter wavelengths. This spectral criterion guarantees that a large proportion of sources will be detected with mas-resolution. This spectral selectiveness is common for almost all previous VLBI surveys and future large VLBA surveys (e.g., VIPS, Taylor et al.~2005, to start in 2006). There are two exceptions, the PR+CJ1 and the Bologna samples. The PR+CJ1 sample (e.g., Person \& Readhead~1988, Xu et~al.~1995) includes all sources with flux density $> 0.7$~Jy at 5~GHz. Unfortunately, only 128 out of 200 were observed with VLBI, so the sample of observed sources is complete only at the 64\% level. Another complete sample of sources, regardless of spectral index value, is the Bologna sample of 95 objects (Giovanni et al.~2004). However this sample, first, limits the objects with redshift $z<0.1$, secondly, only a fraction of these objects has been observed with VLBI. Nevertheless, even preliminary results showed that statistics based on flat-spectrum samples may not give a valid role of compact emission in galaxies and quasars since they ``found a dramatically higher fraction of two-sided sources in comparison with that of previous flux-limited VLBI survey.'' We analyzed statistics of 3989 sources observed in 21 VLBA Calibrator survey experiments, 53 VLBA RDV experiments and 3941 Mark3/Mark4 experiments for geodesy and astrometry and compared it with the complete NVSS catalog (Condon et~al.~1998). According to Table~1, only 20--30\% of sources were observed even among the strong objects with the total flux density $>1$~Jy at 1.4~GHz. \begin{table}[h] \caption{Statistics of observed sources in geodesy and astrometry programs} \begin{center} \begin{tabular}{lrrr} \hline S at 1.4~GHz, Jy & \# total in NVSS & \# observed & \# detected \\ \hline $>$5.0 & 167 & 50 & 44 \\ $>$2.0 & 727 & 198 & 179 \\ $>$1.0 & 2206 & 485 & 446 \\ \hline \end{tabular} \end{center} \end{table} \newpage \section{Scientific Goals} The scientific goal of the proposed campaign is to perform a statistical study of the complete sample of all 500 objects with NVSS flux density at 1.4~GHz $>200$~mJy in the area of 0.21 srad around the northern celestial pole. This sample was chosen because it has been observed with the Russian transit mode radio telescope RATAN--600 in 2005, and simultaneous measurements of total flux density at 2, 5, 8, 11, and 22~GHz are available (Mingaliev et~al.~2001, 2005, in preparation). The proposed observations will identify those sources from this sample which have compact details at the level of 20~mJy or higher at X and/or S bands. We expect that between 100 and 200 sources will be detected (this proportion is really unknown); images and positions at mas level will be obtained. Precise positions will enable performing reliable optical identification and follow-up VLBA studies which are planned for detected sources with mas-scale components. Analysis of this sample should provide insight into the following questions:\\ $\bullet$~~What is the share of CSS in the entire population of AGN? What percentage of compact sources are missed in flat-spectrum surveys? What proportion of the detected sources are radio cores of FR\,I and FR\,II sources?\\ $\bullet$~~Do these CSS that have an overall steeper spectrum have different morphological properties from their flatter-spectrum cousins?\\ $\bullet$~~Do CSS counts and properties change to fainter flux density / luminosity level (e.g., a higher portion of compact sources at low flux density level is suggested by the VLA MASIV survey results, Lovell~et~al.~2003)?\\ $\bullet$~~What is the relationship between the total spectrum of CSS from the RATAN supporting observations and the spectrum of compact components? Are differences related to ageing?\\ $\bullet$~~What is the probability that a source with a given spectral index and total flux density will have a given compactness? Finally, results of this campaign will allow us to determine the true distribution of compact emission and its spectral properties for an unbiased complete sample of sources. This knowledge will allow us to assess whether conclusions drawn from VLBI surveys of flat-spectrum sources can be extended to the whole population of extragalactic objects regardless their continuum spectrum. \section{Proposed Observations} We request three 24~hour observing sessions. Each source will be observed in one scan for 7 minutes. Eight IF channels, four in S-band and four in X-band are proposed, with a total bandwidth of 64~MHz at 1~bit sampling, 128~Mbps. We will reach the 20 mJy detection level and even with the relatively poor $uv$ coverage, images will be made at both frequencies. We will determine the group delays of the detected sources and obtain better positions of the compact emission. We request the same correlator setup as in the BP\,118 proposal: 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. Analysis of BP\,118 observations showed that the a~priori position errors for 20\% of detected sources were greater than 1~arcsec and for 8\% --- greater than 5~arcsec. The observations scheme will be identical to the recent VLBA Calibrator survey experiments. The calibration and imaging will be made by using standard packages AIPS and difmap. Positions will be determined with Calc/Solve. \begin{thebibliography}{} \bibitem[]{r2} Beasley,~A.~J., Gordon,~D., Peck,~A.~B., Petrov,~L., MacMillan,~D.~S., Fomalont,~E.~B., \& Ma,~C.\ 2002, ApJS, 141, 13 \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 \bibitem[]{r4} Fomalont, E.~B., Petrov, L., MacMillan, D.~S., Gordon, D., \& Ma, C.\ 2003, AJ, 126, 2562 \bibitem[]{bologna} Giovanini, G., Taylor, G.~B., Feretti, L., Cotton, W.~D., Lara, L., \& Venturi, T.\ 2005, AJ, 618, 635 %"First Results from MASIV: %The Microarcsecond Scintillation-induced Variability Survey" \bibitem[Lovell et al.(2003)]{Lovell_etal03} Lovell, J.~E.~J., et al.\ %Jauncey, D.~L., Bignall, H.~E., %Kedziora-Chudczer, L., Macquart, J.-P., Rickett, B. J., \& Tzioumis, A.~K.\ 2003, AJ, 126, 1699 \bibitem[]{ncp} Mingaliev, M.~G., Stolyarov, V.~A., Davies, R.~D., Melhuish, S.~V., Bursov, N.A., \& Zhekanis~G.V.\ 2001, A\&A, 370, 78 \bibitem[]{PR} Pearson, T.J. \& Readhead, A.~C.~S.\ AJ, 1988, 328, 114 \bibitem[]{r7} Petrov, L., Kovalev, Y.Y., Fomalont, E.~B., \& Gordon, D.\ 2005a, AJ, 129, 1163 \bibitem[]{r8} Petrov, L., Kovalev, Y.Y., Fomalont, E.~B., \& Gordon, D.\ 2005b, AJ, Submitted, astro-ph/0508506 \bibitem[Taylor et al.(2005)]{VIPS} Taylor, G.~B., et al.\ 2005, ApJS, 159, 27; \verb|http://www.phys.unm.edu/~gbtaylor/VIPS/| \bibitem[]{CJ1} Xu, W., Pearson, T.J. \& Readhead, A.~C.~S., Polatidis, A.~G., \& Wilkinson, P.~N.\ ApJS, 1995, 99, 297 \end{thebibliography} \end{document}