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<div class="moz-cite-prefix">Hi Chia Min,</div>
<div class="moz-cite-prefix"><br>
</div>
<div class="moz-cite-prefix">Related to J1749+5952: I think the from
the statement "The increase in width of the main peak at higher
frequency could be due to a larger fraction of the emission region
coming into view as the height of the emission region decreases"
it isn't particularly clear what you have in mind. Note that an
increasing W50 does not automatically imply there is more emission
from the wings of the profile, it could equally well mean that
there is less emission from the region where the profile peaks.</div>
<div class="moz-cite-prefix"><br>
</div>
<div class="moz-cite-prefix">Maybe instead: <br>
</div>
<div class="moz-cite-prefix"><br>
</div>
<div class="moz-cite-prefix">"The increase in width of the main peak
at higher frequency could be affected by the exact beam pattern of
the pulsar, and pulse longitude dependent spectral index effects."<br>
</div>
<div class="moz-cite-prefix"><br>
</div>
<div class="moz-cite-prefix">I admit the new sentence is not
particularly revolutionary either, but I think it is at least a
bit more explicit in terms of what it means.</div>
<div class="moz-cite-prefix"><br>
</div>
<div class="moz-cite-prefix">Cheers,<br>
Patrick</div>
<div class="moz-cite-prefix"><br>
</div>
<div class="moz-cite-prefix"><br>
</div>
<div class="moz-cite-prefix"><br>
</div>
<div class="moz-cite-prefix">On 08/10/2019 10:35, Chia Min Tan
wrote:<br>
</div>
<blockquote type="cite"
cite="mid:AM6PR0102MB3208D475878A3B6953E54880E09A0@AM6PR0102MB3208.eurprd01.prod.exchangelabs.com">
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Hi everyone</div>
<div style="font-family: Calibri, Arial, Helvetica, sans-serif;
font-size: 12pt; color: rgb(0, 0, 0);">
<br>
</div>
<div style="font-family: Calibri, Arial, Helvetica, sans-serif;
font-size: 12pt; color: rgb(0, 0, 0);">
Thanks to everyone who sent me another round of comments. I've
made changes based on the feedback and it should be almost ready
for submission. I hope to submit by this Friday before I move to
Canada. </div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
<br>
</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
I have quite a few comments about the multi-frequency pulse
profile studies and here are my thoughts about them: </div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
<br>
</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
-On the measurement of scattering, I've only done them for
J1745+1252 and J0210+5845 and not J1810+0705 as Marisa's script
currently only supports profiles that can be modelled as single
Gaussian + scattering exponent.</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
<br>
</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
-I expanded on the definition of w50 and w10 of the pulse
profiles saying that it measures between the outermost
components that have height above 10% and 50% of the maximum of
the profiles. I've also added a scale on the plots of the pulse
profile to show the widths in milliseconds.</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
<br>
</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
-On J1643+1338, I believe it is clear that the profiles at all
frequency consists of two separate components, and I can model
them to show the w50 and the separation between the two
components increases at higher frequencies, which are against
RFM model.</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
<br>
</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
-On J1749+5952, the separation between the two major components
follows RFM, but the individual components seems to be narrower
at lower frequencies. I said it could be a larger portion of the
emission regions came into view at higher frequencies, which
makes the components wider.</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
<br>
</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
I don't expect any more major comments but if you have any
feedback can you let me know by tomorrow?</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
<br>
</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
Thanks</div>
<div style="font-family:Calibri,Arial,Helvetica,sans-serif;
font-size:12pt; color:rgb(0,0,0)">
Chia Min</div>
<hr tabindex="-1" style="display:inline-block; width:98%">
<div id="divRplyFwdMsg" dir="ltr"><font style="font-size:11pt"
face="Calibri, sans-serif" color="#000000"><b>From:</b>
lofarpwg <a class="moz-txt-link-rfc2396E" href="mailto:lofarpwg-bounces@astron.nl"><lofarpwg-bounces@astron.nl></a> on behalf of Chia
Min Tan <a class="moz-txt-link-rfc2396E" href="mailto:chiamin.tan@postgrad.manchester.ac.uk"><chiamin.tan@postgrad.manchester.ac.uk></a><br>
<b>Sent:</b> Friday, September 6, 2019 3:13 PM<br>
<b>To:</b> <a class="moz-txt-link-abbreviated" href="mailto:lofarpwg@astron.nl">lofarpwg@astron.nl</a> <a class="moz-txt-link-rfc2396E" href="mailto:lofarpwg@astron.nl"><lofarpwg@astron.nl></a><br>
<b>Subject:</b> Re: [Lofarpwg] LOTAAS binary pulsar + 20
timing paper</font>
<div> </div>
</div>
<div dir="ltr">
<div id="x_divtagdefaultwrapper" dir="ltr"
style="font-size:12pt; color:rgb(0,0,0);
font-family:Calibri,Helvetica,sans-serif,"EmojiFont","Apple
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<p style="margin-top: 0px; margin-bottom: 0px;margin-top:0;
margin-bottom:0">Hi everyone</p>
<p style="margin-top: 0px; margin-bottom: 0px;margin-top:0;
margin-bottom:0"><br>
</p>
<p style="margin-top: 0px; margin-bottom: 0px;margin-top:0;
margin-bottom:0">I have received quite a few constructive
comments about the paper and have been working on them
over the past few weeks. Thanks to those that have sent me
their feedback.
<br>
</p>
<p style="margin-top: 0px; margin-bottom: 0px;margin-top:0;
margin-bottom:0"><br>
</p>
<p style="margin-top: 0px; margin-bottom: 0px;margin-top:0;
margin-bottom:0">I have actually made quite a few
significant changes to the structure of the paper. I have
rewritten the introduction of the paper to focus more on
observing pulsars at low frequencies instead of a general
introduction to pulsar observations. I have also
reorganise the paper, where I place the observation and
data analysis descriptions in Section 2 and focus on the
various results in other sections. I have also made
changes and additions on various result sections based on
the questions and comments I have received. I've also
added some discussion about the long-term flux density
variation of PSR J1657+3304 and how it is unlikely to be
scintillation.<br>
</p>
<p style="margin-top: 0px; margin-bottom: 0px;margin-top:0;
margin-bottom:0"><br>
</p>
<p style="margin-top: 0px; margin-bottom: 0px;margin-top:0;
margin-bottom:0">I have also received question about
whether to present the binary pulsar PSR J1658+3630 in a
separate paper. My plan now is to present the timing
solution of the pulsar (including coarse modelling of DM
variation to reduce the timing residual) and the average
profile and spectrum. There are many more interesting work
that can be done with the pulsar including modelling the
scintillation properties, study of long term DM and
profile variation, and also possibly to look at the
optical properties of the binary companion. Cees
previously kept some of the raw CV data from the pulsar
with the thought of reprocess them with finer channels for
scintillation studies. I'm not sure if he still have those
data lying around.</p>
<p style="margin-top: 0px; margin-bottom: 0px;margin-top:0;
margin-bottom:0"><br>
</p>
<p style="margin-top: 0px; margin-bottom: 0px;margin-top:0;
margin-bottom:0">If anyone has any comments about the
updated draft please send it to me within two weeks. Also
for those who have sent me feedback, can you confirm if
you want to be on the paper as a co-author and send me
your <span>affiliation</span>?<br>
</p>
<p style="margin-top: 0px; margin-bottom: 0px;margin-top:0;
margin-bottom:0"><br>
</p>
<p style="margin-top: 0px; margin-bottom: 0px;margin-top:0;
margin-bottom:0">Cheers</p>
<p style="margin-top: 0px; margin-bottom: 0px;margin-top:0;
margin-bottom:0">Chia Min<br>
</p>
</div>
<hr tabindex="-1" style="display:inline-block; width:98%">
<div id="x_divRplyFwdMsg" dir="ltr"><font
style="font-size:11pt" face="Calibri, sans-serif"
color="#000000"><b>From:</b> Michael Kramer
<a class="moz-txt-link-rfc2396E" href="mailto:mkramer@mpifr-bonn.mpg.de"><mkramer@mpifr-bonn.mpg.de></a><br>
<b>Sent:</b> Tuesday, August 20, 2019 1:21:51 PM<br>
<b>To:</b> Cees Bassa <a class="moz-txt-link-rfc2396E" href="mailto:cbassa@gmail.com"><cbassa@gmail.com></a><br>
<b>Cc:</b> Chia Min Tan
<a class="moz-txt-link-rfc2396E" href="mailto:chiamin.tan@postgrad.manchester.ac.uk"><chiamin.tan@postgrad.manchester.ac.uk></a>;
<a class="moz-txt-link-abbreviated" href="mailto:lofarpwg@astron.nl">lofarpwg@astron.nl</a> <a class="moz-txt-link-rfc2396E" href="mailto:lofarpwg@astron.nl"><lofarpwg@astron.nl></a><br>
<b>Subject:</b> Re: [Lofarpwg] LOTAAS binary pulsar + 20
timing paper</font>
<div> </div>
</div>
<div>
<div class="x_x_BodyFragment"><font size="2"><span
style="font-size:11pt">
<div class="x_x_PlainText">Dear Chia Min,<br>
<br>
I read the paper and have some comments which are
hopefully useful. Please, let me know if<br>
my handwriting is difficult.<br>
<br>
Please, note my comments about the reference to
spectra paper - which is also relevant for<br>
the census papers (I’ll read those shortly). The
problem with the cited Bates et al. and<br>
Jankowski et al references is, that the spectra in
both papers were derived for a relatively<br>
small frequency range, which is well above the the
LOFAR frequencies. When you make<br>
comparisons it is probably more appropriate to refer
to samples which are drawn from<br>
data covering the whole frequency range. Here the
best reference is probably still Maron et al.<br>
<br>
Anyway, I hope the comments are useful.<br>
<br>
Cheers, Michael<br>
<br>
</div>
</span></font></div>
<div class="x_x_BodyFragment"><font size="2"><span
style="font-size:11pt">
<div class="x_x_PlainText"><br>
<br>
> On 6 Aug 2019, at 15:17, Cees Bassa
<a class="moz-txt-link-rfc2396E" href="mailto:cbassa@gmail.com"><cbassa@gmail.com></a> wrote:<br>
> <br>
> Hi Chia Min,<br>
> <br>
> Thanks for sending the draft around. There's
some nice work in the paper.<br>
> <br>
> Below are comments up to section 4. I'll try to
get my comments on the<br>
> rest of the paper by the end of the week.<br>
> <br>
> Regards,<br>
> Cees<br>
> <br>
> Title:<br>
> <br>
> * The title is perhaps a bit long. Since the
title of Daniele's paper<br>
> was: "LOTAAS: Characterization of 20 pulsars",
you could use<br>
> "LOTAAS: Timing of 21 pulsars", though I agree
that having the<br>
> binary MSP in the title is a plus.<br>
> <br>
> SECTION 1:<br>
> <br>
> * I think the introduction needs a bit more
work. Right now, the<br>
> information motivating this paper (pulsar
properties from timing,<br>
> spectral indices from multi-frequency
follow-up, pulse profile<br>
> evolution) is available, but it is not in a
logical order. My<br>
> suggestion would be that you start with a
general overview of pulsar<br>
> science, which has sofar been predominantly
done at higher<br>
> frequencies and the importance of observing at
lower<br>
> frequencies. You can then provide some
information of low-frequency<br>
> studies of known pulsars (Pilia profiles,
LOFAR Census, MSP Census,<br>
> Sobey RM study). This naturally leads into
LOTAAS as the first real<br>
> low frequency pulsar search, and that this
paper presents some of<br>
> the first timing and multi-frequency results
of pulsars discovered<br>
> at these low frequencies.<br>
> <br>
> SECTION 2:<br>
> <br>
> * In the first paragraph it would be good to
compare the setup of the<br>
> timing observations to that of the search
observations in terms of<br>
> number of stations, bandwidth and integration
time.<br>
> <br>
> * Mention psrchive (with Hotan ref) after
dspsr.<br>
> <br>
> * Did you not use any ROACH data from Jodrell?
Certainly for the<br>
> 334MHz observations the coherent dedispersion
will be important.<br>
> <br>
> * I would also restructure section 2 somewhat,
as right now the<br>
> information is spread about. Perhaps a
subsection for timing<br>
> observations, timing of the binary, and follow
up observations for<br>
> profile evolution and spectral properties.
Another approach would be<br>
> to split it in LOFAR core, Jodrell and GLOW
observations.<br>
> <br>
> * The paragraphs about J1658 are also
confusing, and I think all this<br>
> information can be distilled into a table. You
also need to clarify<br>
> the timing procedure a bit, in that we start
off with binary<br>
> parameters determined from variations in the
spin period (an<br>
> incoherent timing solution), to a coherent
timing solution where you<br>
> account for all rotations of the pulsar. You
might also clarify the<br>
> 'accounting for all rotations' at the start of
section 2 when<br>
> discussing the timing of normal pulsars.<br>
> <br>
> * Table 1: miutes -> minutes<br>
> <br>
> * Table 1: Somewhere in the paper we need to
provide the JXXXX+YY<br>
> names from the LOTAAS overview paper to these
timing names. This<br>
> naturally fits in table 1.<br>
> <br>
> SECTION 3:<br>
> <br>
> * For determining the template, you need to
specify to which profile<br>
> you fitted the von Mises profiles. Was it the
single observation<br>
> with the highest S/N or some average of
profiles?<br>
> <br>
> * Add how many von Mises functions you had to
use (just give the<br>
> minimum and maximum).<br>
> <br>
> * "are split into 2 frequency channels" ->
"are averaged into two<br>
> frequency channels".<br>
> <br>
> * I'm a bit worried by only using two frequency
channels to measure<br>
> DM, as you are using two measurements to
obtain two parameters (TOA<br>
> and DM).<br>
> <br>
> * How were the templates at different
frequencies referenced to<br>
> absolute phase? If scattering or intrinsic
profile evolution is<br>
> present then you could impart a DM offset by
this approach.<br>
> <br>
> * You need to clarify what is meant by a jump.
That is not<br>
> nomenclature that non-pulsar astronomers know.
Also change "Any<br>
> offsets" to "Any time offsets", and perhaps
specify what causes<br>
> these (cable length differences etc).<br>
> <br>
> * In paragraph 2 "In order to...", you may want
to make it clear that<br>
> the dense campaigns were meant to remove
ambiguities in the number<br>
> of pulse rotations between consecutive
observations, and that<br>
> getting phase connection on short timescales
allowed extrapolating<br>
> the timing solution to longer timescales
without introducting<br>
> ambiguities.<br>
> <br>
> * I mentioned this for section 2 as well, but
for the timing solution<br>
> of J1658; explain that you got initial orbital
parameters by<br>
> modelling the spin period variations, and used
those to obtain a<br>
> phase coherent timing solution.<br>
> <br>
> * I am not sure a reference exists for
FITORBIT, in which case you may<br>
> have to explain in a bit more detail what the
software does.<br>
> <br>
> * "... is a low S/N pulsar" is an incorrect
statement. low S/N is a<br>
> property of the telescope, not really the
pulsar. Maybe rewrite to<br>
> "In the initial timing observations of PSR
J1643+1338 it was<br>
> detected at low S/N."<br>
> <br>
> * Section 3 is mixing observations and their
analysis with<br>
> results. This may be a large change, but I
think the first 4<br>
> paragraphs could be joined with section 2 to
make a "Observations<br>
> and timing analysis" section. This resolves
some of the duplicity of<br>
> the statements between section 2 and 3. The
rest of section 3 could<br>
> be called "Timing properties".<br>
> <br>
> Sections 4 and 5 also mix analysis and
results. I think it would be<br>
> more logical to include the first paragraph of
section 4 in section<br>
> 2, and similarly the first few paragraphs of
section 5 also fit<br>
> better in section 2.<br>
> _______________________________________________<br>
> lofarpwg mailing list<br>
> <a class="moz-txt-link-abbreviated" href="mailto:lofarpwg@astron.nl">lofarpwg@astron.nl</a><br>
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<br>
----------------------------------------------------------------------------------------------------------<br>
Prof. Dr. Michael Kramer<br>
Director - Max-Planck-Institut für Radioastronomie,
Bonn, Germany<br>
Professor for Astrophysics - University of
Manchester, UK<br>
Professor (Hon-Prof.) - University of Bonn, Germany<br>
<br>
Address: MPI fuer Radioastronomie<br>
Auf dem Huegel 69<br>
53121 Bonn, Germany<br>
<br>
Phone: +49-228-525-278 (direct)<br>
+49-228-525-299 (secretary)<br>
<br>
EMAIL: <a class="moz-txt-link-abbreviated" href="mailto:mkramer@mpifr-bonn.mpg.de">mkramer@mpifr-bonn.mpg.de</a> /
<a class="moz-txt-link-abbreviated" href="mailto:michael.kramer@manchester.ac.uk">michael.kramer@manchester.ac.uk</a><br>
----------------------------------------------------------------------------------------------------------<br>
<br>
<br>
</div>
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<br>
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<pre class="moz-quote-pre" wrap="">_______________________________________________
lofarpwg mailing list
<a class="moz-txt-link-abbreviated" href="mailto:lofarpwg@astron.nl">lofarpwg@astron.nl</a>
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</pre>
</blockquote>
<p><br>
</p>
<pre class="moz-signature" cols="72">--
Dr. Patrick Weltevrede, senior lecturer in pulsar astrophysics
Jodrell Bank Centre for Astrophysics,
Department of Physics and Astronomy, University of Manchester
Office 3.210 Alan Turing Building
Tel: +44 (0) 16127 54162
Website: <a class="moz-txt-link-freetext" href="http://www.jodrellbank.manchester.ac.uk/">http://www.jodrellbank.manchester.ac.uk/</a>
</pre>
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