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antenna.html

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		@@ -156,9 +156,9 @@ equivalent flux density is the flux density of a radio source that doubles the s
		<td>1</td>
		<td>linear</td>
		<td>primary</td>
		<td>48’</td>
		<td>48’(*)</td>
		<td>[50-80]</td>
		<td>[0.52]</td>
		<td>0.52</td>
		<td>125</td>
		</tr>
		<tr class="row-odd"><td>L</td>
		@@ -166,9 +166,9 @@ equivalent flux density is the flux density of a radio source that doubles the s
		<td>1</td>
		<td>linear</td>
		<td>primary</td>
		<td>11.4’</td>
		<td>11.4’(*)</td>
		<td>25-35</td>
		<td>[0.55]</td>
		<td>0.55</td>
		<td>36</td>
		</tr>
		<tr class="row-even"><td>C-high</td>
		@@ -188,13 +188,13 @@ equivalent flux density is the flux density of a radio source that doubles the s
		<td>Gregorian</td>
		<td>0.8’(**)</td>
		<td>90(**)</td>
		<td>0.45-065</td>
		<td>0.45-0.65</td>
		<td>138(**)</td>
		</tr>
		</tbody>
		</table>
		<p>[ ] is an estimate
		(*) at 6.7 GHz
		(*) at the band’s central frequency
		(**) at 22.3 GHz with opacity 0.1 and ground air temperature of 293K.</p>
		<p>The FWHM beam size, as a function of the frequency f, can be approximated by the following rule: FWHM(arcmin)=19.7/ f(GHz)</p>
		<p>SRT receiver changes are quick, allowing for an efficient frequency agility. The selected receiver is set in its focal position within at most a few minutes.
		@@ -581,41 +581,41 @@ and can be included in the observation schedule.</p>
		</div>
		<div class="section" id="gain-curve-calibration">
		<h2>Gain curve calibration<a class="headerlink" href="#gain-curve-calibration" title="Permalink to this headline">¶</a></h2>
		<p>From the measured gain curves (Gain vs. Elevation), one fits a 2-degree polynomial with the following parameters C0, C1 and C2:</p>
		<ul class="simple">
		<li>L-band</li>
		</ul>
		<p>Values adopted same as Bolli et al (2015)</p>
		<ul class="simple">
		<li>C-band</li>
		</ul>
		<p>From the measured gain curves (Gain vs. Elevation), one fits a 2-degree polynomial with the parameters C0, C1 and C2:</p>
		<p>gain (K/Jy) = C2 El^2 + C1 El + C0</p>
		<table border="1" class="docutils">
		<colgroup>
		<col width="28%" />
		<col width="36%" />
		<col width="36%" />
		<col width="20%" />
		<col width="25%" />
		<col width="29%" />
		<col width="27%" />
		</colgroup>
		<thead valign="bottom">
		<tr class="row-odd"><th class="head">Parameter</th>
		<th class="head">Value (L-band)</th>
		<th class="head">Value (C-band)</th>
		<th class="head">Value (K-band)</th>
		</tr>
		</thead>
		<tbody valign="top">
		<tr class="row-even"><td>C0</td>
		<td>0.5061</td>
		<td>0.545439</td>
		<td>0.505427</td>
		</tr>
		<tr class="row-odd"><td>C1</td>
		<td>0.002390</td>
		<td>0.00525597</td>
		<td>0.00864506</td>
		</tr>
		<tr class="row-even"><td>C2</td>
		<td>-0.000021</td>
		<td>-4.55697e-5</td>
		<td>-6.37184e-5</td>
		</tr>
		</tbody>
		</table>
		<p>L-band: from Orlati et al.</p>
		<p>C-band: valid from 2018.</p>
		<p>K-band: from Prandoni et al. (2017).</p>
		</div>
		@@ -755,7 +755,9 @@ spectra containing the signal from the noise diode (when used).</p>
		<p>Spectral-polarimetric techniques with SRT: <a class="reference external" href="https://arxiv.org/abs/1607.03636">Sardinia Radio Telescope wide-band spectral-polarimetric observations of the galaxy cluster 3C 129</a>.</p>
		<p>ROACH1 backend for baseband data recording and pulsar observations: <a class="reference external" href="http://www.oa-cagliari.inaf.it/area.php?page_id=10&skip=3">OAC Internal Report N. 39</a>.</p>
		<p>SARDARA backend description: <a class="reference external" href="https://www.worldscientific.com/doi/full/10.1142/S2251171718500046">SARDARA</a>.</p>
		<p>Pointing calibration: <a class="reference external" href="http://www.oa-cagliari.inaf.it/area.php?page_id=10&skip=4">Tarchi et al. (2013) OAC Internal Report N. 27</a> & Ricci et al (2016).</p>
		<p>Gain curve calibration at L-band: <a class="reference external" href="http://www.ira.inaf.it/Library/rapp-int/499-16.pdf">Orlati et al.</a>.</p>
		<p>Pointing calibration: <cite>Tarchi et al. (2013) OAC Internal Report N. 27 <http://www.oa-cagliari.inaf.it/area.php?page_id=10&skip=4></cite></p>
		<p><a class="reference external" href="http://www.ira.inaf.it/Library/rapp-int/496-16.pdf">Ricci et al., “A first extented catalogue of pointing/focus calibrators for the Sardinia Radio Telescope”</a>.</p>
		</div>
		<div class="section" id="user-guide-and-observing-modes">
		<h1>User guide and observing modes<a class="headerlink" href="#user-guide-and-observing-modes" title="Permalink to this headline">¶</a></h1>

antenna.rst

+19 −17

Original line number	Diff line number	Diff line
		@@ -86,14 +86,14 @@ equivalent flux density is the flux density of a radio source that doubles the s
		======== ========================= ======= ================= =============== ========== ========== =========== ==========
		Band Frequency coverage (GHz) Feeds Polarization type Focal position Beam size Tsys (K) Gain (K/Jy) Sefd (Jy)
		======== ========================= ======= ================= =============== ========== ========== =========== ==========
		P 0.30 -- 0.36 1 linear primary 48' [50-80] [0.52] 125
		L 1.3 -- 1.8 1 linear primary 11.4' 25-35 [0.55] 36
		P 0.30 -- 0.36 1 linear primary 48'(*) [50-80] 0.52 125
		L 1.3 -- 1.8 1 linear primary 11.4'(*) 25-35 0.55 36
		C-high 5.7 -- 7.7 1 circular beam waveguide 2.7' 32-37() 0.60 43()
		K 18 -- 26 7 circular Gregorian 0.8'() 90() 0.45-065 138(**)
		K 18 -- 26 7 circular Gregorian 0.8'() 90() 0.45-0.65 138(**)
		======== ========================= ======= ================= =============== ========== ========== =========== ==========

		[ ] is an estimate
		(*) at 6.7 GHz
		(*) at the band's central frequency
		(**) at 22.3 GHz with opacity 0.1 and ground air temperature of 293K.

		The FWHM beam size, as a function of the frequency f, can be approximated by the following rule: FWHM(arcmin)=19.7/ f(GHz)
		@@ -276,21 +276,19 @@ The observer should perform a focus calibration before starting an observing ses
		Gain curve calibration
		----------------------

		From the measured gain curves (Gain vs. Elevation), one fits a 2-degree polynomial with the following parameters C0, C1 and C2:
		From the measured gain curves (Gain vs. Elevation), one fits a 2-degree polynomial with the parameters C0, C1 and C2:

		* L-band
		gain (K/Jy) = C2 El^2 + C1 El + C0

		Values adopted same as Bolli et al (2015)

		* C-band
		=========== ============== ================ ===============
		Parameter Value (L-band) Value (C-band) Value (K-band)
		=========== ============== ================ ===============
		C0 0.5061 0.545439 0.505427
		C1 0.002390 0.00525597 0.00864506
		C2 -0.000021 -4.55697e-5 -6.37184e-5
		=========== ============== ================ ===============

		=========== ============== ==============
		Parameter Value (C-band) Value (K-band)
		=========== ============== ==============
		C0 0.545439 0.505427
		C1 0.00525597 0.00864506
		C2 -4.55697e-5 -6.37184e-5
		=========== ============== ==============
		L-band: from Orlati et al.

		C-band: valid from 2018.

		@@ -373,7 +371,11 @@ ROACH1 backend for baseband data recording and pulsar observations: `OAC Interna

		SARDARA backend description: `SARDARA <https://www.worldscientific.com/doi/full/10.1142/S2251171718500046>`_.

		Pointing calibration: `Tarchi et al. (2013) OAC Internal Report N. 27 <http://www.oa-cagliari.inaf.it/area.php?page_id=10&skip=4>`_ & Ricci et al (2016).
		Gain curve calibration at L-band: `Orlati et al. <http://www.ira.inaf.it/Library/rapp-int/499-16.pdf>`_.

		Pointing calibration: `Tarchi et al. (2013) OAC Internal Report N. 27 <http://www.oa-cagliari.inaf.it/area.php?page_id=10&skip=4>`

		`Ricci et al., "A first extented catalogue of pointing/focus calibrators for the Sardinia Radio Telescope" <http://www.ira.inaf.it/Library/rapp-int/496-16.pdf>`_.

		User guide and observing modes
		==============================