In the latter part of the **Installing and getting started** on the UAT wiki, read section on theĢ.1 **Loading data from a CSV file**.
The easiest, or Mac disk images, but TOPCAT is also easy to install on Windows machines.Ĭ. Steps in **Installing and Getting Started** for your system. If you have not installed TOPCAT on your laptop or local machine, follow the Site recently (or at all), briefly review the documents there refer to You will see UAT TOPCAT Docs, click there. When you reach the site, look the bar on the left. LBW.3 Introduction to TOPCAT: the Tool for OPerations on Catalogues And Tables,Īn interactive java graphical program which has been developed by astronomers at the Virtual Astronomical Observatory. For the HI line, what velocity corresponds to the central channel of Board 1 What is 9-level sampling, and why is it advantageous?ĭ. What is the total frequency range that our observations cover when the spectrometerĬ. In "high velocity" mode compare to the spectra we record for the A2010 drift scanī. How does the resolution of the spectra obtain for the LBW observations We use another device called the "interim correlator".Ī. LBW.2 Setting the spectrometer: options, options, optionsįor the A2010 drift scan observations, we use the WAPP spectrometer, but for LBW The final spectrum show both positive and negative flux. When we look very close to the rest frequency of the HI line (1420.4058 MHz), we sometimes see What famous politician once said "However beautiful the strategy, you should What observational consideration(s) led us to hold off a serious campaign of followup observations until now?į. What is the slew speed of the telescope in zenith angle?Į. What is the slew speed of the telecope in azimuth?ĭ. ALFALFA also uses "position switching" of a sort how does that work?Ĭ. Why do we need an "OFF" source observation?ī. This is an HI source? If it is an OH megamaser, what is its redshift?ĭuring the UAT12 workshop, we will begin the ALFALFA followup observing program, usingĪ technique of total-power position switching, also known as "ON-OFF observing".Ī. Suppose we observe a source with a frequency that, if the line is HI, is -1515 km/s. We wanted (deliberately) to observe emission from that line close to its rest frequency, where would What spectral line has a rest frequency of about 1424 MHz? If The ALFALFA bandpass covers 1335-1435 MHz. Give us, at a velocity resolution of 10 km/s? How does that compare to ALFALFA?į. What rms noise (in mJy) will we expect our 3-minute ON-OFF observations to We might imagine that if we observe for a really long time, the noise in the spectrum For the same spectal resolution, how much more sensitive (lower rms) isĪGES than ALFALFA? Hint: use simple scaling!ĭ. The AGES program maps small areas (~10-20 sqd each) using ALFA with anĮffective integration time of 300 seconds. How do we get theĪnswer "40 seconds", i.e. We say that the "effective" integration time for ALFALFA is about 40 seconds per beam. How long does it take a point source to drift across an ALFA beam? Hmmm. January 2012 UAT workshop (as if our annual trips to Puerto Rico weren't already excitingĪ. We'll start these observations during the Now that we have completed most of the ALFALFA drift scan observations, we are initiatingĪ second phase of the survey project to conducted targeted observations of interestingĪLFALFA detections or possible detections. In the writing of the proposal, especially Catherine, Lucas and Wyatt!!! If you have not already done the exercise to examine theĮxample dark objects in α.40 in preparationįor the submission of the observing proposal, we suggest you should do it now. This scavenger hunt will provide an introduction to the point-and-track observations with L-band wide that will be UAT12.01 LBW Scavenger Hunt: Introduction to ALFALFA Followup Observing with L-band Wide Source anywhere but please be sure to indicate where you got your information. With the interim correlator Rules of the scavenger hunts: You may consult any