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<!-- DOI: 10.1051/0004-6361/200911774 -->

<h2 class="sec">Online Material</h2>

<p></p><h2 class="sec"><a name="SECTION00070000000000000000"></a>4&nbsp;Appendix
</h2>

<p></p><div class="inset-old">
<table>
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<td class="img-txt"><span class="bold">Figure A:</span><p>
<b>1 a)</b></td>
</tr>
</table></div><div class="inset-old">
<table>
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<td class="img-txt"><span class="bold">Figure A:</span><p>
<b>1 b)</b> Reproductions of the blue POSS-II survey measure 6' by 6',
north is at top, east at left. The dwarf galaxies FS20 and&nbsp;LeG18
are given in the <i> upper image</i> <b> a)</b>, while d1217+4708 is shown in the <i> lower picture</i>&nbsp;<b> b)</b>.</td>
</tr>
</table></div>Around the position of each galaxy in our sample, we examined a
region of 9.3&nbsp;arcmin radius (i.e., twice the half-power beam width of
the Effelsberg telescope) using the Digital Sky Survey (DSS),
as well as the velocity and other data provided in the NED. Based on
this, if we failed to identify one or more likely sources of confusion with
the observed HI profile, we accepted the HI&nbsp;profile to be genuinely
associated with the targeted dwarf galaxy.<br>

<p><b>d0245+3955, d0245+3957, and d0246+3952</b><br>
 
  These irregular galaxies of low surface brightness form a tight 
triple sub-system inside the NGC&nbsp;1023 group.<br>

</p><p><b>d0946+6842</b><br>

This faint object of very low surface brightness was discovered  by
Chiboucas et&nbsp;al. (<A NAME="aaref2"></A><a href="/articles/aa/full_html/2009/41/aa11774-09/aa11774-09.html#Chiboucas09">2009</a>) as a probable background galaxy behind the
M&nbsp;81 group. There is a strong disagreement between its low luminosity and
the broad HI&nbsp;line width, leading to <IMG SRC="img123.png" ALT="$M_{\rm T}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="23">/<IMG SRC="img3.png" ALT="$L_{\rm B}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="19">
<IMG SRC="img7.png" ALT="$\sim$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="13">
184<A NAME="tex2html13" HREF="#foot628"><sup><IMG ALT="[*]" SRC="/icons/foot_motif.png" align="bottom" BORDER="1"></sup></A> and 
<!-- MATH: $M_{\rm HI}$ -->
<IMG SRC="img2.png" ALT="$M_{\rm HI}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="26">/
<!-- MATH: $L_{\rm B} = 30$ -->
<IMG SRC="img124.png" ALT="$L_{\rm B} = 30$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="49">
in solar units.
 We carefully inspected its surroundings using POSS-II and SDSS
 and did not find any suitable optical counterpart to explain the
 detected HI signal.  This object would be an  interesting target for a more detailed study.<br>

</p><p><b>FS&nbsp;20 = LeG&nbsp;19 and LeG&nbsp;18</b><br>

These dwarf members of the Leo-I group (Karachentsev and
Karachentseva 2004) are separated by <IMG SRC="img7.png" ALT="$\sim$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="13">3 arcmin (see Fig.&nbsp;A.1), 
both being
within the antenna beam. LeG&nbsp;18 was detected within the Arecibo ALFALFA
survey as AGC&nbsp;201970 with 
<!-- MATH: $V_{\rm HI} = 636$ -->
<IMG SRC="img125.png" ALT="$V_{\rm HI} = 636$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="61">&nbsp;km&nbsp;s<sup>-1</sup>, 
<!-- MATH: $W_{50} = 38$ -->
<i>W</i><sub>50</sub> = 38&nbsp;km&nbsp;s<sup>-1</sup>, and <i>S</i> = 0.55&nbsp;Jy&nbsp;km&nbsp;s<sup>-1</sup>. FS&nbsp;20 may be probably
identified with AGC&nbsp;205290 [10 46 42.4 +12 46 58] with 
<!-- MATH: $V_{\rm HI} = 915$ -->
<IMG SRC="img126.png" ALT="$V_{\rm HI} = 915$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="60">&nbsp;km&nbsp;s<sup>-1</sup>, 
<!-- MATH: $W_{50} =50$ -->
<i>W</i><sub>50</sub> =50&nbsp;km&nbsp;s<sup>-1</sup>, and <i>S</i> = 1.46&nbsp;Jy&nbsp;km&nbsp;s<sup>-1</sup> (Stierwalt et&nbsp;al. <a href="/articles/aa/full_html/2009/41/aa11774-09/aa11774-09.html#Stierwalt09">2009</a>). Both objects are within the so-called ``Leo HI ring'' (Schneider et&nbsp;al. <A NAME="aaref17"></A><a href="/articles/aa/full_html/2009/41/aa11774-09/aa11774-09.html#Schneider83">1983</a>).<br>

</p><p><b>CGCG 66-109</b><br>

  This is another dwarf member of the Leo-I group (see Stierwalt et&nbsp;al. <a href="/articles/aa/full_html/2009/41/aa11774-09/aa11774-09.html#Stierwalt09">2009</a>), for which 
<!-- MATH: $V_{\rm HI} = 777$ -->
<IMG SRC="img127.png" ALT="$V_{\rm HI} = 777$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="61">&nbsp;km&nbsp;s<sup>-1</sup>, 
<!-- MATH: $W_{50} = 44$ -->
<i>W</i><sub>50</sub> = 44&nbsp;km&nbsp;s<sup>-1</sup>, and <i>S</i> = 1.74&nbsp;Jy&nbsp;km&nbsp;s<sup>-1</sup>. Its optical velocity, 
<!-- MATH: $982 \pm 78$ -->
<IMG SRC="img40.png" ALT="$982 \pm 78$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="53">&nbsp;km&nbsp;s<sup>-1</sup>, from the SDSS  DR4 corresponds to a blue knot outside the galaxy centre.<br>

</p><p><b>d1150+5546</b><br>

The marginal narrow HI line (
<!-- MATH: $v = 594 \pm 6$ -->
<IMG SRC="img128.png" ALT="$v = 594 \pm 6$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="68">&nbsp;km&nbsp;s<sup>-1</sup>) reported by
Karachentsev et&nbsp;al. (<a href="/articles/aa/full_html/2009/41/aa11774-09/aa11774-09.html#Karachentsev07">2007</a>) lies in a radial velocity range with frequent RFI. Therefore, we included this object in Table&nbsp;<a href="/articles/aa/full_html/2009/41/aa11774-09/aa11774-09.html#tab3">3</a> (upper limits).<br>

</p><p><b>d1217+4703 = BTS&nbsp;109</b><br> This is a new tiny member of the
Canes Venatici&nbsp;I cloud (see Fig.&nbsp;A.1) with very high
HI-mass-to-luminosity ratio of&nbsp;6.5, and <i>M</i><sub><i>T</i></sub>/
<!-- MATH: $L_{\rm B} = 29$ -->
<IMG SRC="img129.png" ALT="$L_{\rm B} = 29$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="50">&nbsp;in solar units.<br>

</p><p><b>d1221+2814 = KK&nbsp;138</b><br>
 
Marginal&nbsp;HI detection. The broad HI line width 
<!-- MATH: $W_{50} = 186$ -->
<i>W</i><sub>50</sub> = 186&nbsp;km&nbsp;s<sup>-1</sup> yields  an extremely high total-mass-to luminosity ratio of <IMG SRC="img7.png" ALT="$\sim$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="13">250 in solar units.<br>

</p><p><b>d1233+3806 = BTS&nbsp;142</b><br>

  This object was detected also in a blind&nbsp;HI survey at Westerbork
(Kovac et&nbsp;al. <A NAME="aaref13"></A><a href="/articles/aa/full_html/2009/41/aa11774-09/aa11774-09.html#Kovac09">2009</a>); 
<!-- MATH: $V_{\rm HI} = 719$ -->
<IMG SRC="img130.png" ALT="$V_{\rm HI} = 719$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="60">&nbsp;km&nbsp;s<sup>-1</sup>, 
<!-- MATH: $W_{50} = 47$ -->
<i>W</i><sub>50</sub> = 47&nbsp;km&nbsp;s<sup>-1</sup>, and  <i>S</i> = 0.41&nbsp;Jy&nbsp;km&nbsp;s<sup>-1</sup>.<br>

</p><p><b>KKSG&nbsp;29</b><br> 

This is a probable dwarf companion of NGC&nbsp;4594 (the ``Sombrero''
galaxy); 
<!-- MATH: $V_{\rm LG} = 828$ -->
<IMG SRC="img131.png" ALT="$V_{\rm LG} = 828$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="64">&nbsp;km&nbsp;s<sup>-1</sup>. Assuming a distance of 9.33&nbsp;Mpc (Ferrarese et&nbsp;al. <A NAME="aaref3"></A><a href="/articles/aa/full_html/2009/41/aa11774-09/aa11774-09.html#Ferrarese00">2000</a>)
for NGC4594 the projected separation of KKSG&nbsp;29 from NGC&nbsp;4594
is 218&nbsp;kpc. A difference in radial velocity of 266&nbsp;km&nbsp;s<sup>-1</sup> between both galaxies yields an orbital mass estimate of 
<!-- MATH: $1.2 \times  10^{13}~M_{\odot}$ -->
<IMG SRC="img132.png" ALT="$1.2 \times 10^{13}~M_{\odot}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="30" WIDTH="82">
or 
<!-- MATH: $M_{\rm orb}$ -->
<IMG SRC="img133.png" ALT="$M_{\rm orb}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="30">/
<!-- MATH: $L_{\rm B}  = 140$ -->
<IMG SRC="img134.png" ALT="$L_{\rm B} = 140$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="56">
in solar units.
There are four other probable dwarf companions to the Sombrero
galaxy within  200&nbsp;kpc, KKSG&nbsp;31, KKSG&nbsp;32, KKSG&nbsp;33, and
 KKSG&nbsp;34; which are all of type dSphs and not detected in&nbsp;HI.<br>

</p><p><b>d1243+2956 = BTS&nbsp;152</b><br>

This object is HI-rich, a suitable target for a detailed study in
H<IMG SRC="img135.png" ALT="$_{\alpha}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="10">
and HI.<br>

</p><p><b>d1243+4127</b><br> 

A new dwarf member of the CVn&nbsp;I cloud. It was also detected by Kovac
et&nbsp;al. (<a href="/articles/aa/full_html/2009/41/aa11774-09/aa11774-09.html#Kovac09">2009</a>) with 
<!-- MATH: $V_{\rm LG} = 436$ -->
<IMG SRC="img136.png" ALT="$V_{\rm LG} = 436$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="63">&nbsp;km&nbsp;s<sup>-1</sup>.<br>

</p><p><b>d1312+4147 = KKH&nbsp;82 = UGCA&nbsp;337</b><br>

A new member of the CVn&nbsp;I cloud. Its optical velocity of 
<!-- MATH: $529 \pm 40$ -->
<IMG SRC="img79.png" ALT="$529 \pm 40$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="54">&nbsp;km&nbsp;s<sup>-1</sup> (SDSS DR4) agrees well with the HI velocity. However,
the broad HI&nbsp;line width of 234&nbsp;km&nbsp;s<sup>-1</sup> yields an extremely high
<IMG SRC="img123.png" ALT="$M_{\rm T}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="23">/
<!-- MATH: $L_{\rm B} = 182$ -->
<IMG SRC="img137.png" ALT="$L_{\rm B} = 182$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="57">
in solar units. No suitable object for confusion could be found within the antenna beam.

</p><p><A NAME="tab3"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/41/aa11774-09/table3.html"><span class="bold">Table 3:</span></a>&#160;&#160;
Observational data - upper limits.</p>
<p></p>
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