\subsection{Applications} The official proposal cover page should be filled in with great care. All information on this page gets directly transferred into the IRAM proposal database. Attention should be given to {\it Other requirements} where the proposer can enter dates where he/she is not available for observing. In order to avoid useless duplication of observations and to protect already accepted proposals, we keep a computerized list of targets. We ask you to fill in carefully the source list in equatorial J2000 coordinates. This list {\it must contain all the sources} (and only those sources) for which you request observing time. Your list must adhere to the format indicated on the proposal form. If your source list is longer than 15 sources that fit onto the cover page, please use the \LaTeX %macro {\tt \begin{verbatim}\extendedsourcelist\end{verbatim}}. macro \verb+\extendedsourcelist+. A scientific project should not be artificially cut into several small projects, but should rather be submitted as one bigger project, even if this means 100--150 hours of observing time. Note that large programs of particular scientific importance can be submitted in the ``Large Programs'' category\ref{Large}. If time has already been given to a project but turned out to be insufficient, explain the reasons, e.g. indicate the amount of time lost due to bad weather or equipment failure; if the fraction of time lost is close to 100\%, don't rewrite the proposal, except for an introductory paragraph. For continuation of proposals having led to publications, please give references to the latter. \subsection{Reminders} For any questions regarding the telescope and the control programs, we recommend to consult the \href{http://www.iram.es/IRAMES/mainWiki/TelescopeSystemSummary} {summary of telescope parameters} and the \href{http://www.iram.es/IRAMES/ncs30m/}{NCS web pages}. The report entitled \href{http://www.iram.es/IRAMES/otherDocuments/manuals/index.html}{Calibration of spectral line data } explains in detail the applied calibration procedure. %A catalog of well calibrated spectra for a range of sources and %transitions (Mauersberger et al. \cite{Mauer}) is very useful for %monitoring spectral line calibration. A copy of the 30m file with the %calibrated spectra can be %\htmladdnormallink{downloaded}{\wwwes/dataarchive/linecal/linecal/init.html} %from the Spanish web site. %The powerful On-the-Fly observing mode (OTF) is available for heterodyne %observations. Documentation is available on the %Granada web page. Due to the complexity of the OTF observing mode %we advise proposers without a demonstrated experience of this technique %on the 30m telescope to contact %, or involve in their proposal, an astronomer with such experience. %*** NAME *** of the Granada staff %(\htmladdnormallink{{\tt ute@iram.es}}{mailto:ute@iram.es}) %serves as the principal contact in OTF matters. The astronomer of duty (see the schedule here: \href{../IRAMES/mainWiki/AstronomerOnDutySchedule}{\wwwes/mainWiki/AstronomerOnDutySchedule}) should be contacted well in advance for any special questions concerning the preparation of an observing run. Frequency switching is available for both HERA and shall also be available for EMIR. This observing mode is interesting for observations of narrow lines where flat baselines are not essential, although the spectral baselines with HERA are among the best known in frequency switching. Certain limitations exist with respect to maximum frequency throw ($\le 45$ km/s), backends, phase times etc.; for a detailed report see \cite{R9}. This report also explains how to identify mesospheric lines which may easily be confused in some cases with genuine astronomical lines from cold clouds. If your observations with the 30m telescope results in a publication, please acknowledge this in a footnote "Based on observations with the IRAM 30-m telescope. IRAM is supported by CNRS/INSU (France), the MPG (Germany) and the IGN (Spain). Please email a copy of the publication to Dennis Downes (downes@iram.fr). %Finally, to help us keeping up a computerized source list, we ask you to fill %in your `list of objects' as explained before. \subsection{Observing time estimates} This matter needs special attention as a serious time underestimate may be considered as a sure sign of sloppy proposal preparation. We strongly recommend to use a new version of ASTRO/GILDAS for time estimates for EMIR, as detailed above, and the old \href{http://www.iram.es/IRAMES/obstime/time_estimator.html}{web--based Time Estimator} for HERA and MAMBO2. %Version~2.6 handles heterodyne (single pixel and HERA) as well as %bolometer observations with updated instrumental parameters. %Suggestions and questions can be addressed to NN (Grewing knows). %(\htmladdnormallink{aweiss@iram.es}{mailto:aweiss@iram.es}). If very special observing modes are proposed which are not covered by the Time Estimator, proposers must give sufficient technical details so that their time estimate can be {\it reproduced}. In particular, the proposal must give values for $T_{\rm sys}$, the spectral resolution, the expected antenna temperature of the signal, the signal/noise ratio which is aimed for, all overheads and dead times, and the resulting observing time. The details of the procedures on which our time estimator is based are explained in a technical report published in the January 1995 issue\protect\footnote{\ electronically available at URL {\tt ../IRAMFR/\-ARN/\-newsletter.html}} of the IRAM Newsletter \cite{R10}. Proposers should base their time request on normal %\textdefsummerwinter{summer}{winter} summer conditions, corresponding to %\textdefsummerwinter{7}{4}mm 7\,mm of precipitable water vapor. Conditions during afternoons can be degraded due to anomalous refraction. The observing efficiency is then reduced and the flux/temperature calibration is more uncertain than the typical 10 percent (possibly slightly more for bolometer observations). If exceptionally good transmission or stability of the atmosphere is requested which may be reachable only in %\textdefsummerwinter{quasi--winter}{best winter} best summer conditions, the proposers must clearly say so in their time estimate paragraph. Such proposals will however be particularly scrutinized. %as they may have to be scheduled in our new priority scheme (see above), %for which only a small fraction of winter time will be reserved. \subsection{Pooled observing} \label{pools} %summer/winter As in previous semesters, we plan to pool the bolometer with other suitable proposals into a bolometer pool. HERA projects will be pooled with other less demanding project into a HERA pool. Both pools will be organized in several sessions, occupying a significant fraction of the totally available observing time. % CKR-CHECK We plan to include EMIR 0.8\,mm observations in these pools. % %As in the previous winters, we plan to reserve a large fraction of the %semester to pooled observing. % The proposals participating in the pools will be observed by % CKR-CHECK the PIs and Co-PIs of participating projects, and IRAM staff. %IRAM and other cooperating external astronomers. % The pool observations will be organized by the pool coordinators, Guillermo Quintana-Lacaci (MAMBO2/1) and Helmut Wiesemeyer (HERA). The participating proposals are grouped according to their demand on weather quality, and they get observed following the priorities assigned by the program committee. The organization of the bolometer and the HERA observing pools are described at \htmladdnormallink {../IRAMES/mainWiki/PoolObserving} {\wwwes/mainWiki/PoolObserving}. Bolometer and heterodyne proposals which are particularly weather tolerant qualify as backup for the pools. Participation in the pools is voluntary, and the respective box on the proposal form should be checked. Questions concerning the pool organization can be directed to the scheduler (thum\mbox{@}iram.fr) or the Pool Coordinators, Guillermo Quintana-Lacaci (quintana\mbox{@}iram.es) and Helmut Wiesemeyer (wiesemeyer\mbox{@}iram.es). \subsection{Service observing} To facilitate the execution of short ($\leq$8 h) programmes, we propose ``service observing'' for some easy to observe programmes {\it with only one set of tunings}. Observations are made by the local staff using precisely laid--out instructions by the principal investigator. %This is a passive way of %observing, no direct interaction with the telescope through OBS being %possible. For this type of observation, we request an acknowledgement of the IRAM staff member's help in the forthcoming publication. If you are interested in this mode of observing, specify it as a ``special requirement'' in the proposal form. IRAM will then decide which proposals can actually be accepted for this mode. \subsection{Remote observing} This observing mode where the remote observer actually controls the telescope very much like on Pico Veleta, is available from the IRAM offices in Granada and Grenoble, and from the MPIfR Bonn and Madrid. If you are planning to use remote observing, please contact the Astronomer on Duty (for Granada), % Pierre Hily--Blant (hilyblan@iram.fr) for Grenoble, % CK-CKR did someone replace Pierre ? % or Dirk Muders, muders@mpifr-bonn.mpg.de for Bonn well in advance of your observing run. As a safeguard, please email observing instructions and macros to the AoD and/or operator. A dedicated phone line to the control desk for voice mail is available for remote observers: +34 958 482009. \subsection{Technical Information about the 30m Telescope} This section gives all the technical details of observations with the 30m telescope that the typical user will have to know. A concise summary of telescope characteristics is published on the \htmladdnormallink{IRAM web pages} {\wwwes/mainWiki/TelescopeSystemSummary}. \subsubsection{HERA} A full description of HERA {\bf HE}terodyne {\bf R}eceiver {\bf A}rray and its observing modes is given in the \htmladdnormallink{HERA manual}{\wwwes/otherDocuments/manuals/HERA_manual_v20.pdf}. Here we only give a short summary. The 9 dual--polarization pixels are arranged in the form of a center--filled square and are separated by $24''$. Each beam is split into two linear polarizations which couple to separate SIS mixers. The 18 mixers feed 18 independent IF chains. Each set of 9 mixers is pumped by a separate local oscillator system. The same positions can thus be observed simultaneously at any two frequencies inside the HERA tuning range (210-276 GHz for the first polarization, and 210-242 for the second polarization). A derotator optical assembly can be set to keep the 9 pixel pattern stationary in the equatorial or horizontal coordinates. Receiver characteristics are listed in Tab.~\ref{Rxs}. Recent observations have shown that the noise temperature of the pixels of the second polarization array may vary across the 1 GHz IF band. The highest noise occurs towards the band edges which are, unfortunately, picked up when HERA is connected with VESPA whose narrow observing band is located close to the lower edge of the 1 GHz band. Therefore, while not as important for wide band observations with centered IF band, the system noise in narrow mode is higher (factor 1.5 -- 2) as compared to the first polarization array. We do not recommend to use the second polarization for frequencies $>241$\,GHz. HERA can be connected to three sets of backends: \begin{itemize}%{$\rhd$} \item[$\rhd$] VESPA with the following combinations of nominal resolution (KHz) and maximum bandwidth (MHz): 20/40, 40/80, 80/160, 320/320, 1250/640. The maximum bandwidth can actually be split into two individual bands for each of the 18 detectors at most resolutions. These individual bands can be shifted separately up to $\pm200$ MHz offsets from the sky frequency (see also the sections on backends below). \item[$\rhd$] a low spectral resolution (4 MHz channel spacing) filter spectrometer covering the full IF bandwidth of 1 GHz. Nine units (one per HERA pixel) are available. Note that only one polarization of the full array is thus connectable to these filter banks. \item[$\rhd$] WILMA with a 1 GHz wide band for each of the 18 detectors. The bands have 512 spectral channels spaced out by 2 MHz. %WILMA will be available after successful completion of the current tests. \end{itemize} HERA is operational in two basic spectroscopic observing modes: {\it (i)} raster maps\footnote{\ As long as the NCS raster command is not operational, the raster pattern has to be traced out with the help of a SIC loop.} of areas typically not smaller than $ 1'$, in position, wobbler, or frequency switching modes, and {\it (ii)} on--the--fly maps of moderate size (typically $2' - 10'$). Extragalactic proposals should take into account the current limitations of OTF line maps, as described in the HERA User Manual, due to baseline instabilities induced by residual calibration errors. HERA proposers should use the web--based \htmladdnormallink{Time Estimator}{\wwwes/obstime/time_estimator.html}. For details about observing with HERA, consult the User manual. The HERA project scientist, Karl Schuster (schuster\mbox{@}iram.fr), or Albrecht Sievers (sievers\mbox{@}iram.es), the astronomer in charge of HERA, may also be contacted. Accepted HERA proposals will be pooled together in order to make more efficient use of stable 1.3mm observing conditions (see section~\ref{pools}. Questions concerning the HERA pool organization can be directed to the scheduler (thum\mbox{@}iram.fr) or the HERA Pool Coordinator, Helmut Wiesemeyer (wiesemeyer\mbox{@}iram.es). \subsubsection{EMIR} see the special section above %\subsubsection{The single pixel heterodyne receivers} % %Four dual polarization SIS receivers are available at the telescope %for the upcoming observing season. They are designated according to %the dewar in which they are housed (A, B, C, or D), followed by the %center frequency (in GHz) of their tuning range. Their main %characteristics are summarized in Tab.~\ref{Rxs}. All receivers are %linearly polarized with the E--vectors, before rotation in the %Martin--Puplett interfero\-meters, either horizontal or vertical in %the Nasmyth cabin. Up to four of these eight receivers can be %combined for simultaneous observations in the four ways depicted in %Tab.~\ref{Rxs}. Note that they cannot be combined with HERA nor with %the bolometers. Also listed are typical system temperatures which %%apply to average %%\textdefsummerwinter{summer weather (7mm of water)}{winter weather (4mm)} %summer/winter weather (7mm/4mm of water) at the center of the tuning %range and at 45\degr\ elevation. All receivers are tuned by the %operators from the control room. Experience shows that it normally %takes not more than 15 min to tune four such receivers. % %\input{tableWinter} % %According to current planning IRAM will replace the present set single %pixel heterodyne receivers by a new generation receiver designated %EMIR ({\bf E}ight {\bf MI}xer {\bf R}eceiver). EMIR is expected to be %installed during the second half of the winter semester. Because this %time scale is still somewhat uncertain and the EMIR characteristics %are not yet precisely known, we request observers to still use the %characteristics of the present receivers for their proposals. %Observations scheduled after the installation of EMIR may get their %time allocation adjusted accordingly. % % % %\paragraph{Extended tuning range: 72 -- 80 GHz.} % %Several molecules of high astrophysical importance have transitions %in the frequency band 66 -- 80 GHz, i.e. between the atmospheric %$O_2$ absorption band and the low frequency edge of the nominal 3mm %tuning range (see Tab.\ref{Rxs}). Tests have shown that both 3mm %receivers, A\,100 and B\,100 have good performance (good upper %sideband rejection and system temperature) in the range 77 --- 80 %GHz. The receivers become increasingly double sideband %below 77 GHz, until their behavior becomes erratic around 72 GHz. %Due to the rapid variation of the image gain, special care must be %exercised with calibration. A new image gain calibration tool is %provided and described in the test report available on the %\htmladdnormallink{IRAM web site} {\wwwfr/veleta.htm} (at %../IRAMFR/PV/veleta.htm). The report includes a set of reference spectra. % %Observations in the 72 -- 80 GHz range do not require any special %arrangements. But note that the A\,230 (B\,230) receiver is not %available when the A\,100 (B\,100) receiver is used below 80 GHz. %\paragraph{General point about receiver operations.} % %% CK-CHECK: Clemens, is the following still needed. %% Could you provide a list of frequencies to be prepared by SN,DJ %% from the schedule db? % %Tuning of the single pixel/dual polarization receivers is now %considerably faster and more reproducible than before. Particular %frequencies, like those in the range 72 -- 80 GHz or those near a %limit of the tuning range, may still be problematic. In these cases, %we request to check with a Granada receiver engineers at least two %weeks before the observations. HERA observers, however, are requested %to send their frequencies as soon as their project gets scheduled. %% %\paragraph{Polarimeter XPOL.} %% not offered with EMIR, at least not this semester % %%An \htmladdnormallink{IF polarimeter}{\wwwold/$\tilde{}$\,thum/spie.ps.gz} %An upgrade of the IF polarimeter \htmladdnormallink{\cite{IFpol}} %{\www/~thum/spie.ps.gz} is now available, %%for observations of compact sources. %where the cross correlation between the IF signals from a pair of orthogonally %polarized receivers is made digitally in VESPA. %The new observing procedure, designated XPOL, generates simultaneous %spectra of all 4 Stokes parameters. The following combinations of %spectral resolution (kHz) and bandwidth (MHz) are available: %40/120, 80/240, and 320/480. %, and 1250/640. %%A few hardware and software complications still exist %%(involving manual wiring of LO cables and manual phase calibration) %%which are expected to be solved early in the next semester. %Although successful XPOL observations were made at many frequencies, %experience is still limited, particularly at 1.3mm wavelength and %with respect to observations of extended sources. %Considerable progress was made in reducing polarization sidelobes, notably %for Stokes V. Interested users should contact C.~Thum for details. %Data reduction software using CLASS enhanced with a %graphical user interface is available (\htmladdnormallink{H.~Wiesemeyer} %{wiesemey\mbox{@}iram.es}). The technical aspects of XPOL and its %observing capabilities and limitations are described in ref.~\ref{XPOL}. %%\htmladdnormallink{Thum et al. 2008} %%{http://adsabs.harvard.edu/abs/2008PASP..120..777T}. %Polarimetry proposals for observation of extended sources should demonstrate %that their observations are feasible in the presence of the known %sidelobes. \subsubsection{MPIfR Bolometer arrays} The bolometer arrays, \Mone\ (37 pixels) and \Mtwo\ (117 pixels), are provided by the Max--Planck--Institut f\"ur Radioastronomie. They consist of concentric hexagonal rings of horns centered on the central horn. Spacing between horns is $\simeq 20''$. Each pixel has a HPBW of 11$''$. We expect that \Mtwo\ will be normally used, but \Mone\ is kept as a backup. The effective sensitivity of both bolometers for onoff observations is %\textdefsummerwinter{39}{$\sim35$} $\sim 40$ mJy\,s$^\frac{1}{2}$ and $\sim45$ mJy\,s$^\frac{1}{2}$ for mapping. The {\it rms}, in mJy, of a \Mtwo\ map is typically $$ rms = 0.4 f \sqrt{v_{scan} \Delta s} $$ where $v_{scan}$, in arc\,sec/sec, is the velocity in the scanning direction and $\Delta s$, in arc\,sec, is the step size in the orthogonal direction. The factor $f$ is 1 (2) for sources of size $<30''\ (>60'')$. It is assumed that the map is made large enough that all beams cover the source. %Since in the mapping mode all beams cover the inner region of the map %area, \Mtwo\ turns out to be more sensitive if areas of $2'$ and larger %are to be mapped (see the Time Estimator). The sensitivities apply to bolometric %\textdefsummerwinter{conditions (stable atmosphere}{winter conditions} conditions (stable atmosphere), ($\tau(\small{250{\rm GHz}})\sim$ %\textdefsummerwinter{0.3}{0.25}, 0.3, elevation 45 deg, and application of skynoise filtering algorithms). In cases where skynoise filtering algorithms are not or not fully effective (e.g. extended source structure, atmosphere not sufficiently stable), the effective sensitivity is typically about a factor of 2 worse. %For those projects, only atmospheric conditions with %low skynoise (i.e. stable atmosphere, no clouds, %little turbulence) are recommened unless the %expected signal is about 1 Jy/beam or stronger. The principal investigators of accepted proposals will be requested to specify in the pool database which minimum atmospheric conditions their observations need. The bolometer arrays are mostly used in two basic observing modes, ON/OFF and mapping. Previous experience with \Mtwo\ shows that the ON/OFF reaches typically an rms noise of $\sim2.3$ mJy in 10 min of total observing time (about 200 sec of ON source, or about 400 sec on sky integration time) under stable conditions. Up to 30 percent lower noise may be obtained in perfect weather. In this observing mode, the noise integrates down with time $t$ as $\sqrt{t}$ to rms noise levels below 0.4 mJy. In the mapping mode, the telescope is scanning in the direction of the wobbler throw (default: azimuth) in such a way that all pixels see the source once. % and fully sample the beam. A typical single map\footnote{\ see also the Technical report by D.~Teyssier and A.~Sievers on a special fast mapping mode (IRAM Newsletter No.~41, p.~12, Aug.~1999).} with \Mtwo\ covering a fully and homogeneously sampled area of $150''\times150''$ (scanning speed: $5''$per sec, raster step: $8''$) reaches an rms of 2.8 mJy/beam in 1.9 hours if skynoise filtering is effective. Much more time is needed (see Time Estimator) if sky noise filtering cannot be used. The area actually scanned ($8.0'\times6.5'$) must be larger than the map size (add the wobbler throw and the array size ($4'$), the source extent, and some allowance for baseline determination) if the EHK--algorithm is used to restore properly extended emission. Shorter scans may lead to problems in restoring extended structure. Mosaicing is also possible to map larger areas. Under many circumstances, maps may be co--added to reach lower noise levels. %but this may require very sophisticated data reduction %(please contact the experts). %Attempts to reach map noise levels below 1 mJy %are still fraught with poorly understood problems If maps with an rms$\simlt1$ mJy are proposed, the proposers should contact R.~Zylka (zylka\mbox{@}iram.fr). %Another note of caution: mapping of extended sources cannot rely on the %skynoise reduction algorithm (simple subtraction of correlated sky-noise) %presently available, and the noise level reached may be at least %twice as high as that quoted above. The bolometers are used with the wobbling secondary mirror (wobbling at a rate of 2 Hz). %The wobbling direction which used to be %fixed in azimuth, can now be freely chosen within some limits (see %IRAM Newsletter No.~61). This allows in virtually all cases to adapt %the wobbling/scanning direction to the source under study. %Nevertheless, t The orientation of the beams on the sky changes with hour angle due to parallactic and Nasmyth rotations, as the array is fixed in Nasmyth coordinates and the wobbler direction is fixed with respect to azimuth during a scan. Bolometer proposals participating in the pool have their observations (maps and ONOFFs) pre-reduced by a data quality monitor which runs scripts in %the newly developed MOPSIC. This package, complete with all necessary scripts, is also installed for off-line data analysis in Granada and Grenoble. It is also available for distribution from the IRAM Data Base for Pooled Observations or directly from R. Zylka (zylka\mbox{@}iram.fr). The older software packages (NIC \cite{R12} and MOPSI \cite{R13}) are still available, but %will not be updated. %Time estimators for planning ON/OFF or mapping observations are also available %\cite{R12,TE2}. cannot process data obtained with the NCS. Bolometer proposals will be pooled together like in previous semesters along with suitable heterodyne proposals as long as the respective PIs agree. %Their time requests should be based on %``bolometric conditions'', %like requests using SIS receivers, The web--based time estimator handles well the usual bolometer observing modes, and its use is again strongly recommended. The time estimator uses rather precise estimates of the various overheads which will be applied to all bolometer proposals. If exceptionally low noise levels are requested which may be reachable only in a perfectly stable %\textdefsummerwinter{(quasi winter)}{(perfect winter)} (quasi winter) atmosphere, the proposers must clearly say so in their time estimate paragraph. Such proposals will however be particularly scrutinized. On the other extreme, if only strong sources are observed and moderate weather conditions are sufficient, the proposal may be used as a backup in the observing pool. The proposal should point out this circumstance, as it affects positively the chance that the proposal is accepted and observed. %\subsubsection{The 2mm bolometer} %DIABOLO which currently employs a linear 3 pixel array at 2mm is designed %for detection of weak and somewhat extended sources. The instrument which %was used successfully at the 30m telescope last winter, is %described by X.~D\'esert %elsewhere in this newsletter. The level of integration %of the instrument into the 30m telescope's standard control and acquisition %system is minimal, however, complicating the use of this instrument. %Obervers interested in using DIABOLO should contact %X.~D\'esert at the Observatoire de Grenoble for arranging some form of %collaboration. \subsection{The Telescope} \subsubsection{Beam and Efficiencies} See the \href{http://www.iram.es/IRAMES/mainWiki/TelescopeSystemSummary} {summary of telescope parameters} for the current efficiencies between 70 and 270~GHz, and the predictions for the 345~GHz (0.8~mm) band. %% Much of the following is badly outdated, in contrast to the wiki!! CK-CHECK %Table~\ref{t:eff} lists the size of the telescope beam for the %range of frequencies of interest. Forward and main beam efficiencies %are also shown (see also the note by U.~Lisenfeld and A.~Sievers, IRAM %Newsletter No.~47, Feb. 2001). The variation of the %coupling efficiency to sources of different sizes can be estimated from %plots in Greve et al. \cite{beam}. % %At 1.3 mm (and a fortiori at shorter wavelengths) a large %fraction of the power pattern is distributed in an error %beam which can be approximated by two Gaussians of FWHP $\simeq 170''$ %and $800''$ (see \cite{beam} for details). %Astronomers should take into account this error beam when converting %antenna temperatures into brightness temperatures. % %% CKR-CHECK: the following is a bit outdated: %A variable and sometimes large contribution to the error beam was known %to come from telescope astigmatism \cite{R7}. %Extensive work during the last years had shown that the astigmatism resulted %from temperature differences between the telescope backup structure and %the yoke. The recent installation of heaters in the yoke by J.~Pe\~{n}alver %has nearly completely removed the astigmatism \cite{astigmatism}. % %The aperture efficiency depends somewhat on the elevation, particularly %at shorter wavelengths. This gain/elevation effect is evaluated in \cite{g/e}. % %\begin{table} %\caption{Main observational parameters of 30m telescope.}\label{t:eff} %Forward and main beam efficiencies, $\eta_F$ and $\eta_{mb}$, % and beam width $\theta_b$ (FWHP).} %\vspace{1ex} %\begin{center} %\begin{tabular}{|ccccc|}\hline % frequency & $\theta_b$ [''] & $\eta_F$ & % $\eta_{mb}$ \rule{0em}{3ex} & $S_\nu$/T$_A^{\ast}$\\[0.4ex] %[GHz] & (1) & (2) & (3) & [Jy/K] \\[1ex]\hline % 86 & 29 & 0.95 & 0.78 & 6.0\rule{0em}{3ex}\\ % 110 & 22 & 0.95 & 0.75 & 6.3\\ % 145 & 17 & 0.93 & 0.69 & 6.7\\ % 170 & 14.5 & 0.93 & 0.65 & 7.1\\ % 210 & 12 & 0.91 & 0.57 & 7.9\\ % 235 & 10.5 & 0.91 & 0.51 & 8.7\\ % 260 & 9.5 & 0.88 & 0.46 & 9.5\\ % 279 & 9 & 0.88 & 0.42 & 10.4\\[1ex]\hline %\end{tabular} %\end{center}% % %(1) beam width (HPBW). A fit to all data gives:\rule{0em}{3ex} % \makebox[1.5em]{}$\theta_b$ [''] = 2460 / frequency [GHz]\\ %(2) forward efficiency (coupling efficiency to sky) \\ %(3) main beam efficiency. Based on a fit of measured % \makebox[1.5em]{}data to the Ruze formula:\\ % \makebox[1.5em]{}$\eta_{\rm mb}=1.2\epsilon \exp(-(4\pi R \sigma/\lambda)^2)$\\ % \makebox[1.5em]{}with $\epsilon=0.69$ and $R\sigma=0.07$\\ %(4) in units of Jy/K %\end{table} \subsubsection {Pointing and Focusing} With the systematic use of inclinometers the telescope pointing became much more stable. Pointing sessions are now scheduled at larger intervals. %Pointing sessions are normally scheduled twice per week; at present, The fitted pointing parameters typically yield an absolute rms pointing accuracy of better than $3''$ \cite{pointing}. However, larger deviations can occur around sunset or sunrise, in which case we recommend more frequent pointings (every 1 or 2 hours, depending on the beam size). An effort is made that receivers are closely (usually $\simlt2''$) aligned. %, however, alignment can be lost occasionally). Checking the pointing, focus, and receiver alignment is the responsibility of the observers (use a planet for alignment checks). Systematic (up to 0.4 mm) differences between the foci of various receivers %were noted in the past and may well persist, even with the new %generation receivers. can occasionally occur. In such a case the foci should be carefully monitored and a compromise value be chosen. Not doing so may result in broadened and distorted beams (\cite{R2}). %\begin{table} %\caption[]{Summary of 30m telescope characteristics} %\label{summ} %\begin{tabular}{|c|}\hline %supplied by Wolfgang\\ \hline %\end{tabular} %\end{table} \subsubsection {Wobbling Secondary} \begin{itemize} \item Beam--throw is $\le 240''$ depending on wobbling frequency. At 2 Hz, the maximum throw is $90''$ \item Standard phase duration: 2 sec for spectral line observations, 0.25 sec for continuum observations. \end{itemize} Unnecessarily large wobbler throws should be avoided, since they introduce a loss of gain, particularly at the higher frequencies, and imply a loss of observing efficiency (more dead time). \subsection{Backends} \label{ss:backends} The following five spectral line backends are available which can be individually connected to any single pixel receiver and, if indicated, also to HERA. {\bf The 1 MHz filterbank} consists of 4 units. Each unit has 256 channels with 1~MHz spacing and can be connected to different or the same receivers giving bandwidths between 256 MHz and 1024 MHz. The maximum bandwidth is available for only one receiver, naturally one having a 1 GHz wide IF bandwidth. Connection of the filterbank in the 1~GHz mode presently excludes the use of any other backend with the same receiver. Other configurations of the 1 MHz filterbank include a setup in 2 units of 512 MHz connected to two different receivers, or 4 units of 256 MHz width connected to up to four (not necessarily) different receivers. Each unit can be shifted in steps of 32 MHz relative to the center frequency of the connected receiver. %% CKR-CHECK: not offered anymore: %{\bf The 100 kHz filterbank} consists of 256 channels of 100 kHz spacing. %It can be split into two halves, each movable inside the 500 MHz IF %bandwidth, and connectable to two different single pixel receivers %(must be set up in narrow band mode). %{\bf The autocorrelator backend} with up to 2048 channels. %Available nominal resolutions are 10, 20, 40, 80, 320 and 1250 KHz. %Nominal bandwidths range from 20 MHz to $2\times 512$ MHz, %depending on resolution. The correlator can be split into 8 %independent subbands, each of which can be configured individually, shifted %inside a 500 MHz IF band, and %connected to the same or different receivers. For the larger %bandwidths (i.e. more than one subband of 80 MHz) there is often a problem of %platforming, i.e. baselines from the different subbands have %slightly different power levels. {\bf VESPA}, the versatile spectrometric and polarimetric array, can be connected either to HERA or to a subset of 4 single pixel receivers, or to a pair of single pixel receivers for polarimetry. The many VESPA configurations and user modes are summarized in a \htmladdnormallink{Newsletter contribution}{\www/ARN/dec02/node6.html} \cite{vespasummary} and in a \htmladdnormallink{user guide}{\wwwes/otherDocuments/manuals/vespa_ug.ps}, but are best visualised on a demonstration program which can be downloaded from \htmladdnormallink{our web page}{\wwwfr/veleta.htm} at URL \wwwfr/veleta.htm. Connected to a set of 4 single pixel receivers, VESPA typically provides up to 12\,000 spectral channels (on average 3\,000 per receiver). Up to 18\,000 channels are possible in special configurations. Nominal spectral resolutions range from 3.3 kHz to 1.25 MHz. Nominal bandwidths are in the range 10 --- 512 MHz. When VESPA is connected to HERA, up to 18\,000 spectral channels can be used with the following typical combinations of nominal resolution (kHz) and maximum bandwidth (MHz): 20/40, 40/80, 80/160, 320/320, 1250/640. {\bf The 4 MHz filterbank} consists of nine units. Each unit has 256 channels (spacing of 4 MHz, spectral resolution at 3 dB is 6.2 MHz) and thus covers a total bandwidth of 1 GHz. The 9 units are designed for connection to HERA, but a subset of 4 units can also be connected to the backend distribution box which feeds the single pixel spectral line receivers. All these receivers have a 1~GHz RF bandwidth except for A100 and B100 (500 MHz only). %At the present time, a 4 MHz filterbank cannot be used simultaneously with %the autocorrelator or the 100 kHz filterbank on the same receiver. %The raw data from these filterbanks are written to a Linux %workstation. An off--line calibration macro is available for the basic %observing modes (PSWITCH, WSWITCH, RASTER), but automatic %calibration is being prepared. Frequency switching is %not possible with these low resolution backends. (*** is all that still true?) %An on--line calibration routine automatically writes calibrated %spectrometer data, including the 4 MHz filterbanks, %%Now the on-line reduced data for %to the Linux machines. The routine, although still experimental, works %for all observing modes. %, including On--the--Fly. %A logical link named ``data.30m'' pointing to this file of calibrated spectra %is made available in all newly created project accounts. The {\bf wideband autocorrelator WILMA} consists of 18 units. They can be connected to the 18 detectors of HERA. Each unit provides 512 spectral channels, spaced out by 2 MHz and thus covering a total bandwidth of 1 GHz. Each band is sliced into two 500 MHz subbands which are digitized with 2~bit/1~GHz samplers. An informative technical overview of the architecture is available at URL \htmladdnormallink{../IRAMFR/\-TA/backend/veleta/\-wilma/index.htm} {/IRAMFR/TA/backend/veleta/wilma/index.htm}. % Note that WILMA cannot presently be connected to any of the single pixel receivers. %\item The 500 channel AOS: ({\em Under repair})\\ %Bandwidth 500 MHz; actual spectral %resolution 1.5 MHz. Using the AOS with the 3 mm SIS receiver results %in higher noise at the band edges, so the combination 3 mm SIS + AOS %is not recommended. \begin{thebibliography}{99} %\bibitem{R1} Receiver tests during the August 1992 period\\ % M. Carter, J.Y. Chenu, H. Hein, S. Navarro, A. Greve, M. Gu\'elin %(Sept 92) \bibitem{R2} Appendix I: Error beam and side lobes of the 30 m telescope at 1.3 mm, 2 mm and 3 mm wavelength, in ``Molecular Spiral Structure in Messier 51'',\\ S. Garcia-Burillo, M. Gu\'elin, J. Cernicharo 1993, Astron. Astrophys. {\bf 274}, 144-146. \bibitem{R3} A Small Users' Guide to NOD2 at the 30m telescope A. Sievers (Feb. 1993) %\bibitem{R4} Thermal behaviour of mm-wavelength radio telescopes %\\ A. Greve, M. Dan, J. Pe\~{n}alver %1992 (IRAM report 233) %1993, IEEE Trans. Ant. Propag. AP--40, 1375 %\bibitem{R5} Interferometric measurement of tropospheric phase %fluctuations at 86 GHz\\ L. Olmi, D. Downes 1992 (IRAM report 238) %\bibitem{R6} Thermal design and thermal behaviour of Radio %Telescope structures\\ A. Greve 1992 (IRAM report 253) \bibitem{R7} Astigmatism in reflector antennas: measurement and correction\\ A. Greve, B. Lefloch, D. Morris, H. Hein, S. Navarro %1993 (IRAM report 289) 1994, IEEE Trans. Ant. Propag. AP--42, 1345 %\bibitem{R8} Design parameters and measured performance of the %IRAM 30m millimeter radio telescope\\ J. Baars, A. Greve, H. Hein, D. %Morris, J. Pe\~{n}alver, C. Thum %1993 (IRAM report 298). %1993, Proc. IEEE~82, 687 \bibitem{R9} \htmladdnormallink{Frequency switching at the 30m telescope} {\wwwes/otherDocuments/manuals/Report/} \\ C. Thum, A. Sievers, S. Navarro, W. Brunswig, J. Pe\~nalver 1995, IRAM Tech. Report 228/95. \\(\wwwes/\-otherDocuments/\-manuals/\-Report/fsw\_doc.ps) \bibitem{R10} Cookbook formulae for estimating observing times at the 30m telescope \\ M.~Gu\'elin, C.~Kramer, and W.~Wild\\ (\htmladdnormallink{IRAM Newsletter January 1995} {\www/ARN/jan95/jan95.html}) \bibitem{R11} The 30m Manual: A Handbook for the 30m Telescope (version~2), W.~Wild 1995 \\IRAM Tech. Report~377/95,\\ also available on the web at \htmladdnormallink{../IRAMES/\-otherDocuments/\-manuals/\-manual\_v20.ps} {\wwwes/otherDocuments/manuals/manual_v20.ps} \bibitem{R12} NIC: Bolometer User's Guide \\D. Brogui\`ere, R. Neri, A. Sievers, and H.~Wiesemeyer 2000, IRAM Technical Report (\htmladdnormallink{../IRAMFR/\-GILDAS/\-doc/\-html/\-nic-html/\-nic.html} {\www/IRAMFR/\-GILDAS/\-doc/\-html/\-nic-html/\-nic.html});\\ \mbox{see also the \htmladdnormallink{GILDAS home page} {/IRAMFR/\-GILDAS/} at} /IRAMFR/\-GILDAS/ with further relevant technical reports. \bibitem{R13} Pocket Cookbook for MOPSI software %\\\mbox{R. Zylka 1996, available at} \\R. Zylka 1996, available at\hfill \htmladdnormallink {../IRAMES/otherDocuments/manuals/ \\Datared/pockcoo.ps} {\wwwes/\-otherDocuments/\-manuals/\-Datared/pockcoo.ps}. \bibitem{Mauer} Line Calibrators at $\lambda =$ 1.3, 2, and 3mm. \\R.~Mauersberger, M.~Gu\'elin, J.~Mart{\'\i}n--Pintado, C.~Thum, J.~Cernicharo, H.~Hein, and S.Navarro 1989, A\&A Suppl. 79, 217 \bibitem{pointing} The Pointing of the IRAM 30m Telescope \\A.~Greve, J.--F.~Panis, and C.~Thum 1996, A\&A Suppl. 115, 379 \bibitem{g/e} The gain--elevation correction of the IRAM 30m Telescope \\A.~Greve, R.~Neri, and A.~Sievers 1998, A\&A Suppl. 132, 413 \bibitem{beam} The beam pattern of the IRAM 30m Telescope \\A.~Greve, C.~Kramer, and W.~Wild 1998, A\&A Suppl. 133, 271 \bibitem{TE2} A Time Estimator for Observations at the IRAM 30m Telescope, D.~Teyssier 1999, IRAM/Granada Technical Note (\wwwes/\-obstime/\-time\_estimator.html) \bibitem{vespasummary} Short guide to VESPA G.~Paubert %\\IRAM Newsletter No.~54, 6 %\\(\wwwfr/veleta.htm and \wwwes\-/otherDocuments\-/manuals/\-vespa\_ug.ps) \bibitem{astigmatism} First results from the IRAM 30m telescope improved thermal control system \\J.~Pe\~{n}alver, A.~Greve, and M.~Bremer 2002, IRAM Newsletter No.~54, 8 \bibitem{IFpol}A Versatile IF Polarimeter at the IRAM 30m Telescope\\ C.~Thum, H.~Wiesemeyer, D.~Morris, S.~Navarro, and M.~Torres\\ in ``Polarimetry in Astronomy'', Ed. S.Fineschi, Proc.of SPIE Vol.4843, 272--283 (2003) \bibitem{XPOL} XPOL -- the correlation polarimeter at the IRAM 30m telescope\\ Thum, C., Wiesemeyer, H., Paubert, G., Navarro, S., and Morris, D.\\ \htmladdnormallink{PASP 120, 777 (2008)} {http://adsabs.harvard.edu/abs/2008PASP..120..777T} \end{thebibliography} These reports are available upon request (see also previous Newsletters). Please write to Mrs. C. Berjaud, IRAM Grenoble (e--mail: {\tt berjaud\mbox{@}iram.fr}). \signed{ %\htmladdnormallink{Clemens Thum}{mailto:thum@iram.fr}, %\htmladdnormallink{Rainer Mauersberger}{mailto:mauers@iram.es}} Clemens Thum \& Carsten Kramer} %\end{document}