<html><head><meta http-equiv="Content-Type" content="text/html charset=big5"></head><body style="word-wrap: break-word; -webkit-nbsp-mode: space; -webkit-line-break: after-white-space;" class=""><div class="">Dear Adam,</div><div class=""><br class=""></div><div class="">I obtained the approval from Roger Cappallo, and I would like to post his comments following this post.</div><div class=""><br class=""></div><div class="">By Roger Cappallo:</div><div class="">—————————————————</div><div class=""><div class="">I looked into a similar synthetic data correlation. </div><div class="">It had 2.000 seconds of data, but showed up on the fourfit plot as an integration</div><div class="">time of 1.984 sec, for both auto- and cross-correlations alike.</div><div class="">Looking into the model used, it turned out that the (single station</div><div class="">to earth center) delay was in fact about 16 ms, consistent</div><div class="">with Adam’s hypothesis about the propagation time delay</div><div class="">being the culprit.</div><div class=""><br class=""></div><div class="">Digging into the correlator output (Swinburne file) data, though,</div><div class="">it turns out that the data weight for the 1st second was</div><div class="">0.984, while the weight for the 2nd second was 1.000, for</div><div class="">a sum of 1.984. fourfit uses these weights to calculate integration</div><div class="">time, thus the final result of 1.984 seconds.</div><div class=""><br class=""></div><div class="">So, for my case it appears that the artifact is indeed coming </div><div class="">from difx, and not from the hops part of the data-processing chain.</div><div class=""><br class=""></div><div class="">I suspect the same is true for your example, though a bit of</div><div class="">digging through your files is required to prove it. More simply,</div><div class="">though Adam might be able to explain why the weight of the</div><div class="">first AP is decreased by the earth-center propagation delay.</div><div class=""><br class=""></div><div class="">For completeness, here are two different ways to find the </div><div class="">necessary evidence, either in the difx or hops world:</div><div class=""><br class=""></div><div class="">****** difx-based (e.g. for fileset h_1000):</div><div class=""><br class=""></div><div class="">propagation delay can be found in the h_1000.im file as </div><div class="">the first term of the quintic delay spline, say by grepping</div><div class="">for DELAY:</div><div class="">grep DELAY h_1000.im</div><div class=""><br class=""></div><div class="">data weights can be found by inspecting the Swinburne file</div><div class="">in the .difx directory, e.g. by using the utility program dumpvis</div><div class="">to create an ASCII copy, and then grepping for weight</div><div class=""><br class=""></div><div class="">****** hops-based (e.g. for fileset suffix uvwxyz and baseline AB):</div><div class=""><br class=""></div><div class="">propagation delay splines are in the type 301 records,</div><div class="">and can be examined with:</div><div class="">CorAsc2 301 < A..uvwxyz | grep delay</div><div class=""><br class=""></div><div class="">data weights are in the type 120 records, and can be</div><div class="">looked at with:</div><div class="">CorAsc2 120 < AA..uvwxyz | grep weight</div></div><div class=""><br class=""></div><div class=""><br class=""></div><div class=""><div class="">dumpvis actually resides in the hops part of the directory structure. </div><div class="">It should be accessible in the hops executables area. For example,</div><div class="">on my system that would be $HOPS_ROOT/i686-3.15/bin</div><div class=""><br class=""></div><div class="">dumpvis is a "quick and dirty” utility, which shows up</div><div class="">in the fact that you have to specify the number of visibilities,</div><div class="">instead of having it infer it from the data. A typical run might be</div><div class="">dumpvis <long-swinburne-file-name> 128 | less</div><div class="">or of course redirecting into a file for later inspection.</div><div class=""><br class=""></div><div class="">The number of visibility points, 128 in this example, is half of</div><div class="">the number of lags at the bottom of the fourfit plot. You</div><div class="">could also find it empirically by trying different powers of</div><div class="">2, and seeing which one doesn’t cause a hiccup at the</div><div class="">2nd record (this is easier and quicker than it sounds).</div><div class=""><br class=""></div><div class="">Rather than looking at the Swinburne file you could of</div><div class="">course use CorAsc2 to inspect the type 120’s.</div></div><div class="">—————————————————</div><div class=""><br class=""></div><div class="">Cheers,</div><div class=""><span style="font-family: 新細明體, sans-serif; font-size: 12px;" class="">--</span></div><div apple-content-edited="true" class=""><div class=""><div style="font-family: 新細明體, sans-serif; font-size: 14px;" class=""><span style="font-size: 12px;" class="">Lupin Chun-Che Lin</span></div><div style="font-family: 新細明體, sans-serif; font-size: 14px;" class=""><span style="font-size: 12px;" class="">Supporting Scientist of GLT (GreenLand Telescope) project </span></div><div style="font-family: 新細明體, sans-serif; font-size: 14px;" class=""><span style="font-size: 12px;" class="">in Institute of Astronomy and Astrophysics, Academia Sinica,</span></div><div style="font-family: 新細明體, sans-serif; font-size: 14px;" class=""><span style="font-size: 12px;" class="">14F of Astronomy-Mathematics Building (Rm: 1405), </span></div><div style="font-family: 新細明體, sans-serif; font-size: 14px;" class=""><span style="font-size: 12px;" class="">National Taiwan University. </span></div><div style="font-family: 新細明體, sans-serif; font-size: 14px;" class=""><span style="font-size: 12px;" class="">No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan.</span></div><div style="font-family: 新細明體, sans-serif; font-size: 14px;" class=""><span style="font-size: 12px;" class="">Tel: +886-2-2366-5464</span></div><div style="font-family: 新細明體, sans-serif; font-size: 14px;" class=""><span style="font-size: 12px;" class="">Fax: +886-2-2367-7849</span></div></div><div class=""><br class=""></div><br class="Apple-interchange-newline">
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<br class=""><div><blockquote type="cite" class=""><div class="">Adam Deller <<a href="mailto:adeller@astro.swin.edu.au" class="">adeller@astro.swin.edu.au</a>> 於 2017年6月10日 上午9:39 寫道：</div><br class="Apple-interchange-newline"><div class=""><div dir="ltr" class="">Hi Lupin,<div class=""><br class=""></div><div class="">For the benefit of the whole difx-users list, I'm copying into this thread my response to you that expanded on the potential cause of reduced weight of the first integration:</div><div class=""><br class=""></div><div class=""><div class="">Data files are recorded at the station in the station's reference frame. Correlation is performed in a geocentric reference frame. If the correlation is to start at time X, the first sample that will be requested by the correlator from the station for the correlation will be at time X-\tau_g, where \tau_g is the geometric delay from the station to the geocentre (to obtain the sample that would have arrived at time X on a plane that passes through the geocentre and is perpendicular to the source direction). And if the station data file starts at exactly time X (same time as the requested correlation start, at the geocentre), then the first \tau_g samples won't be available - they are from before the station started recording. And hence the completeness of the first integration will be less than 1.</div><div class=""><div style="font-size:12.8px" class=""><br class=""></div><div style="font-size:12.8px" class="">If the station started recording one or more seconds prior to the start of the correlation time, then the necessary data will be available and the first integration will have full weight.</div><div style="font-size:12.8px" class=""><br class=""></div><div style="font-size:12.8px" class="">This is not an error on the part of the correlator: it is expected behaviour, and an unavoidable result of time-tagging the visibilities at the geocentre properly. In the astronomical VLBI schedules that I am familiar with, the scheduling software generally forces the stations to start recording a few seconds prior to the intended scan start (or in the event of a small gap between scans, they never stop recording at all), and this issue doesn't arise.</div></div></div><div style="font-size:12.8px" class=""><br class=""></div><div style="font-size:12.8px" class="">Cheers,</div><div style="font-size:12.8px" class="">Adam</div><div class=""><br class=""></div></div><div class="gmail_extra"><br class=""><div class="gmail_quote">On 24 May 2017 at 12:21, Lupin Lin <span dir="ltr" class=""><<a href="mailto:lupin@asiaa.sinica.edu.tw" target="_blank" class="">lupin@asiaa.sinica.edu.tw</a>></span> wrote:<br class=""><blockquote class="gmail_quote" style="margin:0 0 0 .8ex;border-left:1px #ccc solid;padding-left:1ex"><div style="word-wrap:break-word" class=""><div class=""><div class="">Dear Adam,</div><div class=""><br class=""></div><div class="">Thanks for your response again.</div><div class=""><br class=""></div><div class=""><span class=""><blockquote type="cite" class=""><div dir="ltr" class=""><div class=""><div class=""><div class="">But so you've got two datastreams which you've generated from noise sources, is that right? </div></div></div></div></blockquote></span><div class="">Yes.</div></div><div class=""><br class=""></div><div class=""><span class=""><blockquote type="cite" class=""><div dir="ltr" class=""><div class=""><div class=""><div class="">They have independent noise and a common signal which has a small but non-zero delay? </div></div></div></div></blockquote></span>Yes</div><div class=""><br class=""></div><div class=""><span class=""><blockquote type="cite" class=""><div dir="ltr" class=""><div class=""><div class=""><div class="">And then you're putting both data streams into DiFX and saying they are from the same physical position, so they get the same delay model applied. How are you calculating the single phase number? Is that a simple average over the whole band?</div></div></div></div></blockquote></span>The phase value was given by the result shown by fourfit/HOPS.</div><span class=""><div class="">And it "should be” the average of phase distribution shown in Avgd. Power Spectrum over the whole band (Please refer to the attached Zoom_128_5sec.pdf. </div></span></div></div><br class=""><div style="word-wrap:break-word" class=""><div class=""><div class=""></div><div class="">According to the result shown for the cross-correlation, the phase value is -115.4 degree. It is the phase number indicated in my previous “phase.pdf”.) </div><div class=""><br class=""></div><div class=""><blockquote type="cite" class=""><div dir="ltr" class=""><div class=""><div class=""><div class="">What if you reduce the amplitude of the common noise source to something a bit more realistic, like a maximum of 1% of the independent noise amplitude?</div></div></div></div></blockquote>Thanks for the comments, and we will try it. </div><div class=""> </div><div class=""><blockquote type="cite" class=""><div dir="ltr" class=""><div class=""><div class="">I don't have an explanation for why the phase differs between an LO of 86000 MHz vs 220000 MHz when you're extracting a 128 MHz subband, but I can only point the finger at quantisation + numerical precision effects coupled with the very high degree of correlation that appears to be present in your setup.</div></div></div></blockquote>"220 GHz" should be a typo because I set for 230 GHz.</div><div class="">Is there any experiment that we can/should do to further confirm the origin of my problem?</div><div class=""><br class=""></div><div class=""><br class=""></div><div class="">Sincerely,</div><div class=""><div class=""><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">--</span></div><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">Lupin Chun-Che Lin</span></div><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">Supporting Scientist of GLT (GreenLand Telescope) project </span></div><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">in Institute of Astronomy and Astrophysics, Academia Sinica,</span></div><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">14F of Astronomy-Mathematics Building (Rm: 1405), </span></div><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">National Taiwan University. </span></div><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan.</span></div><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">Tel: <a href="tel:+886%202%202366%205464" value="+886223665464" target="_blank" class="">+886-2-2366-5464</a></span></div><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">Fax: <a href="tel:+886%202%202367%207849" value="+886223677849" target="_blank" class="">+886-2-2367-7849</a></span></div></div></div></div><div class=""><br class=""></div><br class=""><div class=""><blockquote type="cite" class=""><div class="">Adam Deller <<a href="mailto:adeller@astro.swin.edu.au" target="_blank" class="">adeller@astro.swin.edu.au</a>> 於 2017年5月22日 上午10:39 寫道：</div><br class="m_-5116304605100313295Apple-interchange-newline"><div class=""><div dir="ltr" class=""><div class=""><div class=""><div class=""><div class="">Hi Lupin,<br class=""><br class=""></div>OK, I think I partly understand now. But so you've got two datastreams which you've generated from noise sources, is that right? They have independent noise and a common signal which has a small but non-zero delay? And then you're putting both data streams into DiFX and saying they are from the same physical position, so they get the same delay model applied. How are you calculating the single phase number? Is that a simple average over the whole band? The changing amplitudes due to the requantisation plus the phase ripple could easily account for some of the differences. It also seems like your S/N is absurdly high, which is probably exacerbating a lot of the quantisation-related effects. What if you reduce the amplitude of the common noise source to something a bit more realistic, like a maximum of 1% of the independent noise amplitude?<br class=""><br class=""></div>I don't have an explanation for why the phase differs between an LO of 86000 MHz vs 220000 MHz when you're extracting a 128 MHz subband, but I can only point the finger at quantisation + numerical precision effects coupled with the very high degree of correlation that appears to be present in your setup.<br class=""><br class=""></div>Cheers,<br class=""></div>Adam<br class=""><div class=""><div class=""><div class=""><div class=""><br class=""></div></div></div></div></div><div class="gmail_extra"><br class=""><div class="gmail_quote">On 22 May 2017 at 12:12, Lupin Lin <span dir="ltr" class=""><<a href="mailto:lupin@asiaa.sinica.edu.tw" target="_blank" class="">lupin@asiaa.sinica.edu.tw</a>></span> wrote:<br class=""><blockquote class="gmail_quote" style="margin:0 0 0 .8ex;border-left:1px #ccc solid;padding-left:1ex"><div style="word-wrap:break-word" class=""><div class="">Dear Adam,</div><div class=""><br class=""></div><div class="">Thanks for your repsonse to give the indication.</div><div class="">For the 1st question, I will further check with the expert of HOPS developer.</div><div class=""><br class=""></div><div class="">For my 2nd question, the Jan’s code is “m5subband” provided in the latest DiFX version to extract the specific frequency range information from a wide/full band data.</div><div class="">The original input is also the 2-bit VDIF file. </div><div class="">I just compare with "the cross-correlation with two 2-bit wide band VDIF files at a specific frequency range using the zoom-band mode" and "one data subtracted a the same frequency range to cross-correlate another wide band file supported with zoom-band mode.”</div><div class="">A simple expression in the .v2d file is the comparison between:</div><div class="">(XXXXX and OOOOO are data with 2 GHz, and SSSSS is a data with the band of 256 MHz subtracted from XXXXX)</div><div class="">————————————————————————</div><div class="">ANTENNA G1</div><div class=""><div class="">{</div><div class=""> file = XXXXX.vdif</div><div class=""> format = VDIF/8224/2</div><div class=""> phaseCalInt = 0</div><div class=""> addZoomFreq= freq@230000.00/bw@256.0</div><div class="">}</div></div><div class=""><div class="">ANTENNA G2</div><div class="">{</div><div class=""> file = OOOOO.vdif</div><div class=""> format = VDIF/8224/2</div><div class=""> phaseCalInt = 0</div><div class=""> addZoomFreq= freq@230000.00/bw@256.0</div><div class="">}</div></div><div class="">———————————————————————— And,</div><div class=""><div class="">ANTENNA G1</div><div class=""><div class="">{</div><div class=""> file = SSSSS.vdif</div><div class=""> format = VDIF/8224/2</div><div class=""> phaseCalInt = 0</div><div class="">}</div></div><div class=""><div class="">ANTENNA G2</div><div class="">{</div><div class=""> file = OOOOO.vdif</div><div class=""> format = VDIF/8224/2</div><div class=""> phaseCalInt = 0</div><div class=""> addZoomFreq= freq@230000.00/bw@256.0</div><div class="">}</div></div></div><div class="">———————————————————————— </div><div class=""><br class=""></div><div class="">The loss in SNR or the amplitude is expected due to the re-sampling (FFT and IFFT for the original XXXXX.vdif) of the data, but we do not clearly understand the origin to cause the "possible shift" in the obtained phase distribution.</div><div class="">(We suspect the shift in phase is due to the adoption of the Ref. Freq., but the series of my tests cannot confirm this point.)</div><div class=""><br class=""></div><div class="">The motivation to do it is that we have limited/very slow internet speed in GLT. </div><div class="">In order to check the preliminary result via the obtained observation, we would like to send only the band reduced data with a much smaller file size.</div><div class="">So to investigate/handle the comparison between the aforementioned two cases is required for GLT team.</div><span class=""><div class=""><br class=""></div><div class="">Sincerely,</div><div class=""><span style="font-family:新細明體,sans-serif;font-size:12px" class="">--</span></div><div class=""><div class=""><div style="font-family:新細明體,sans-serif;font-size:14px" class=""><span style="font-size:12px" class="">Lupin Chun-Che Lin</span></div><div style="font-family:新細明體,sans-serif;font-size:14px" class=""><span style="font-size:12px" class="">Supporting Scientist of GLT (GreenLand Telescope) project </span></div><div style="font-family:新細明體,sans-serif;font-size:14px" class=""><span style="font-size:12px" class="">in Institute of Astronomy and Astrophysics, Academia Sinica,</span></div><div style="font-family:新細明體,sans-serif;font-size:14px" class=""><span style="font-size:12px" class="">14F of Astronomy-Mathematics Building (Rm: 1405), </span></div><div style="font-family:新細明體,sans-serif;font-size:14px" class=""><span style="font-size:12px" class="">National Taiwan University. </span></div><div style="font-family:新細明體,sans-serif;font-size:14px" class=""><span style="font-size:12px" class="">No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan.</span></div><div style="font-family:新細明體,sans-serif;font-size:14px" class=""><span style="font-size:12px" class="">Tel: <a href="tel:+886%202%202366%205464" value="+886223665464" target="_blank" class="">+886-2-2366-5464</a></span></div><div style="font-family:新細明體,sans-serif;font-size:14px" class=""><span style="font-size:12px" class="">Fax: <a href="tel:+886%202%202367%207849" value="+886223677849" target="_blank" class="">+886-2-2367-7849</a></span></div></div><div class=""><br class=""></div><br class="m_-5116304605100313295m_5095474439037212162Apple-interchange-newline">
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<br class=""></span><div class=""><div class="m_-5116304605100313295h5"><div class=""><blockquote type="cite" class=""><div class="">Adam Deller <<a href="mailto:adeller@astro.swin.edu.au" target="_blank" class="">adeller@astro.swin.edu.au</a>> 於 2017年5月22日 上午8:15 寫道：</div><br class="m_-5116304605100313295m_5095474439037212162Apple-interchange-newline"><div class=""><div dir="ltr" style="font-family:Helvetica;font-size:14px;font-style:normal;font-variant:normal;font-weight:normal;letter-spacing:normal;line-height:normal;text-align:start;text-indent:0px;text-transform:none;white-space:normal;word-spacing:0px" class="">Hi Lupin,<br class=""><div class="gmail_extra"><br class=""><div class="gmail_quote">On 19 May 2017 at 13:22, Lupin Lin<span class="m_-5116304605100313295m_5095474439037212162Apple-converted-space"> </span><span dir="ltr" class=""><<a href="mailto:lupin@asiaa.sinica.edu.tw" target="_blank" class="">lupin@asiaa.sinica.edu.tw</a><wbr class="">></span><span class="m_-5116304605100313295m_5095474439037212162Apple-converted-space"> </span>wrote:<br class=""><blockquote class="gmail_quote" style="margin:0px 0px 0px 0.8ex;border-left-width:1px;border-left-color:rgb(204,204,204);border-left-style:solid;padding-left:1ex"><div style="word-wrap:break-word" class="">To the experienced user of DiFX or HOPS,<div class=""><br class=""></div><div class=""><div class="">Sorry to spend you some time on two questions.</div><div class="">The first one is related to the integration time presented on the final plot after the auto- or cross- correlations.</div><div class="">(The DiFX I used is trunk ver. and and the HOPS ver. I used is 3.13)</div><div class=""><br class=""></div><div class="">1. </div><div class="">Here the GLT team recorded two signals with 3 noise sources (only 1 is the same with a potential delay less than 1 ns) from the same ROACH, and made a test in correlation.</div><div class="">We simply assumed that the Sky (Ref.) frequency is 230 GHz and the data were obtained from the same site (both G1 and G2 were assigned to the same position of GLT). </div><div class="">We correlated the data of 5-sec. supported with the zoom-band mode at 1,200-1,328 MHz.</div><div class="">————(Contents in .v2d file)———</div><div class=""><div class="">vex = ext.vex.obs</div><div class="">mjdStart = 2017y124d05h42m00s</div><div class="">mjdStop = 2017y124d05h42m05s</div><div class="">antennas = G1,G2</div><div class="">startSeries = 7000</div><div class="">dataBufferFactor = 16</div><div class="">visBufferLength = 80</div><div class="">nDataSegments = 8</div><div class="">minLength = 0.5</div></div><div class="">————————————————</div><div class="">But according to the attached figure of “Zoom128_5sec.pdf”, the int time is only 4.995 sec.</div><div class="">What’s the reason to cause a loss of the obtained Int. time? </div><div class=""></div></div></div><br class=""></blockquote><div class=""><br class=""></div><div class="">This may be HOPS-related: I'm not an expert on HOPS so I can't comment. But another possibility is that the correlation runs from 054200 to 054205 at the geocentre, and if the recorded data duration was only 5 seconds long but at the telescope, then the geometric delay will mean than a few milliseconds of data will be chopped off. Maybe one of the HOPS users can chime in on how that integration time number is calculated in the HOPS plot - is it based on the weight? If so then my hypothesis is plausible.<br class=""></div><div class=""> </div><blockquote class="gmail_quote" style="margin:0px 0px 0px 0.8ex;border-left-width:1px;border-left-color:rgb(204,204,204);border-left-style:solid;padding-left:1ex"><div style="word-wrap:break-word" class=""><div class=""><div class=""></div><div class=""><br class=""></div><div class="">2. </div><div class="">Following the previous test, I used Jan Wagner’s code to do the band subtraction (the original full band is 2GHz) and checked the obtained phase of different cases.</div><div class="">I summarized my tests and my questions in the attached file “phase.pdf”.</div><div class=""></div></div></div><br class=""><div style="word-wrap:break-word" class=""><div class=""><br class=""><div class=""></div><div class="">The 1st case is the same as shown in the attached “Zoom128_5sec.pdf”.</div><div class="">What’s the possible origin to cause the phase shift? </div><div class="">I originally suspect that such a shift is originated from the change in Sky/Ref. freq, but it might be wrong….</div><div class=""><br class=""></div></div></div></blockquote><div class=""><br class=""></div><div class="">I'm sorry, but I can't follow what your are trying to do here. I'm not sure what Jan's code is that you're referring to (is it something that filters e.g. your 2 GHz band down to 128 MHz in a chosen window?) If that is the case, what is the input - already quantised 2 bit VDIF data? That will lead to nasty re-quantisation errors - you'll notice that the amplitude goes down, too. <span class="m_-5116304605100313295m_5095474439037212162Apple-converted-space"> </span><br class=""><br class=""></div><div class="">But the root of the problem is: what are you actually ultimately trying to achieve? A verification of some kind?<br class=""><br class=""></div><div class="">Cheers,<br class=""></div><div class="">Adam<br class=""></div><div class=""> </div><blockquote class="gmail_quote" style="margin:0px 0px 0px 0.8ex;border-left-width:1px;border-left-color:rgb(204,204,204);border-left-style:solid;padding-left:1ex"><div style="word-wrap:break-word" class=""><div class=""><div class=""></div><div class="">Sincerely,</div><div class=""><div class=""><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">--</span></div><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">Lupin Chun-Che Lin</span></div><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">Supporting Scientist of GLT (GreenLand Telescope) project </span></div><div style="font-family:新細明體,sans-serif" class=""><span style="font-size:12px" class="">in Institute of Astronomy and Astrophysics, Academia 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<br class=""></blockquote></div><br class=""><br clear="all" class=""><div class=""><br class=""></div>-- <br class=""><div class="gmail_signature" data-smartmail="gmail_signature"><div dir="ltr" class=""><div class=""><div dir="ltr" class=""><div class=""><div dir="ltr" class=""><div dir="ltr" class=""><div dir="ltr" class=""><div dir="ltr" class=""><div dir="ltr" class=""><div dir="ltr" style="font-size:12.8000001907349px" class=""><div dir="ltr" style="font-size:12.8px" class=""><div dir="ltr" style="font-size:12.8px" class=""><div dir="ltr" style="font-size:12.8px" class=""><div dir="ltr" style="font-size:12.8px" class="">!=============================================================!<br class="">Dr. Adam Deller </div><div dir="ltr" style="font-size:12.8px" class="">ARC Future Fellow, Senior Lecturer</div><div style="font-size:12.8px" class="">Centre for Astrophysics & Supercomputing </div><div dir="ltr" style="font-size:12.8px" class="">Swinburne University of Technology <br class="">John St, Hawthorn VIC 3122 Australia</div><div style="font-size:12.8px" class="">phone: +61 3 9214 5307</div><div style="font-size:12.8px" class="">fax: +61 3 9214 8797</div><div style="font-size:12.8px" class=""><br class=""></div><div style="font-size:12.8px" class="">office days (usually): Mon-Thu<br class="">!=============================================================!</div></div></div></div></div></div></div></div></div></div></div></div></div></div></div>
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