latest

paper/paper.tex

@@ -203,8 +203,8 @@ \section{Introduction}
 Motivated by observations of other CDGs
   that show gas kinematics ranging from pure rotation and low velocity
 dispersion to high velocity dispersion without a clear rotation pattern
-\citep{2015A&A...577A..21C,2017A&A...600A.125C} we perform here a new
-study to explain \tol's \lya emission features under two physical
+\citep{2015A&A...577A..21C,2017arXiv170809407C,2017A&A...600A.125C}
+we perform here a new study to explain \tol's \lya emission features under two physical
 conditions for the interstellar medium: multiphase outflows and pure rotation.
 
 
@@ -605,10 +605,13 @@ \subsection{Multiphase ISM}
 Under these conditions we find $\sigma_{\rm cl}=$\sigmaclump,
 $v_{\infty {\rm, cl}}=$\inftyclump\ and $P_{\rm cl}=$\probaclump, 
   with the minimum $\chi^2/d.o.f.=11.7$. {\bf This relatively high value
-    could be interpreted as low statistical significance.
-However, we stress once more that this is the first time that the main
+    for the reduced $\chi^2$ could be interpreted as low statistical
+    significance. 
+However, we stress once more that the is the first time that the main
 features of \tol\ can be reproduced, making this model an useful tool
-to guide the interpretation of complex observational data.} 
+to guide the interpretation of complex observational data. 
+These results certainly open up the path to future searches to
+construct new models.} 
 
 Qualitatively this result can be understood as follows.
 Due to the large fraction of \lya photons being emitted within the
@@ -700,7 +703,7 @@ \section{Discussion}
 
 Which model could be closer to the actual kinematic conditions in \tol?  
 Integral Field Unit (IFU) observations of other CDGs seem to
-favor the multiphase model \citep{2015A&A...577A..21C,2017A&A...600A.125C}. 
+favor the multiphase model \citep{2015A&A...577A..21C,2017arXiv170809407C,2017A&A...600A.125C}.
 These observations  were performed with the Visible Multi-Object Spectrograph (VIMOS)
 \citep{2003SPIE.4841.1670L}.
 The spatial sampling was $0.67^{\prime\prime}$ and covered about
@@ -791,7 +794,7 @@ \section{Conclusions}
 \lya emission line.
 One model is based on a multiphase ISM with random clump motions and
 the other on gas bulk solid body rotation. 
-It is the first time that an observed \lya profile can be fully
+It is the first time that an observed \lya profile can be 
 reproduced by either of these two kinematic conditions.
 Our findings highlight the importance of including multiphase and/or
 rotation conditions as kinematic features to model the \lya line.
@@ -829,7 +832,6 @@ \section*{Acknowledgments}
 (\url{http://daft-pgm.org/}).  
 
 \bibliographystyle{mnras}
-%\bibliography{references}
 \begin{thebibliography}{}
 \makeatletter
 \relax
@@ -868,8 +870,15 @@ \section*{Acknowledgments}
 
 \bibitem[\protect\citeauthoryear{{Cair{\'o}s} \&
   {Gonz{\'a}lez-P{\'e}rez}}{{Cair{\'o}s} \&
-  {Gonz{\'a}lez-P{\'e}rez}}{2017}]{2017A&A...600A.125C}
-{Cair{\'o}s} L.~M.,  {Gonz{\'a}lez-P{\'e}rez} J.~N.,  2017, \mn@doi [\aap]
+  {Gonz{\'a}lez-P{\'e}rez}}{2017a}]{2017arXiv170809407C}
+{Cair{\'o}s} L.~M.,  {Gonz{\'a}lez-P{\'e}rez} J.~N.,  2017a, preprint, \href
+  {http://adsabs.harvard.edu/abs/2017arXiv170809407C} {} (\mn@eprint {arXiv}
+  {1708.09407})
+
+\bibitem[\protect\citeauthoryear{{Cair{\'o}s} \&
+  {Gonz{\'a}lez-P{\'e}rez}}{{Cair{\'o}s} \&
+  {Gonz{\'a}lez-P{\'e}rez}}{2017b}]{2017A&A...600A.125C}
+{Cair{\'o}s} L.~M.,  {Gonz{\'a}lez-P{\'e}rez} J.~N.,  2017b, \mn@doi [\aap]
   {10.1051/0004-6361/201629681}, \href
   {http://adsabs.harvard.edu/abs/2017A%26A...600A.125C} {600, A125}
 
@@ -884,9 +893,6 @@ \section*{Acknowledgments}
 {Dey} A.,  {Spinrad} H.,  {Stern} D.,  {Graham} J.~R.,   {Chaffee} F.~H.,
   1998, \mn@doi [\apjl] {10.1086/311331}, \href
   {http://adsabs.harvard.edu/abs/1998ApJ...498L..93D} {498, L93}
-  
-\bibitem[Dijkstra et al.(2006)]{2006ApJ...649...14D} Dijkstra, M., Haiman, Z., \& Spaans, M.\ 2006, \apj, 649, 14 
-
 
 \bibitem[\protect\citeauthoryear{{Dijkstra}}{{Dijkstra}}{2014}]{2014PASA...31...40D}
 {Dijkstra} M.,  2014, \mn@doi [\pasa] {10.1017/pasa.2014.33}, \href
@@ -1071,7 +1077,6 @@ \section*{Acknowledgments}
   {Terlevich} R.~J.,   {Terlevich} E.,  2003, \mn@doi [\apj] {10.1086/379116},
   \href {http://adsabs.harvard.edu/abs/2003ApJ...598..858M} {598, 858}
 
-
 \bibitem[\protect\citeauthoryear{{McKee} \& {Ostriker}}{{McKee} \&
   {Ostriker}}{1977}]{1977ApJ...218..148M}
 {McKee} C.~F.,  {Ostriker} J.~P.,  1977, \mn@doi [\apj] {10.1086/155667}, \href
@@ -1240,6 +1245,8 @@ \section*{Acknowledgments}
 \makeatother
 \end{thebibliography}
 
+%\bibliography{references}
+
 
 
 \appendix

paper/references.bib

@@ -53,6 +53,21 @@ @INPROCEEDINGS{2003SPIE.4841.1670L
   adsnote = {Provided by the SAO/NASA Astrophysics Data System}
 }
 
+
+@ARTICLE{2017arXiv170809407C,
+   author = {{Cair{\'o}s}, L.~M. and {Gonz{\'a}lez-P{\'e}rez}, J.~N.},
+    title = "{Probing star formation and feedback in dwarf galaxies. Integral field view of the blue compact galaxy Tololo 1937-423}",
+  journal = {ArXiv e-prints},
+archivePrefix = "arXiv",
+   eprint = {1708.09407},
+ keywords = {Astrophysics - Astrophysics of Galaxies},
+     year = 2017,
+    month = aug,
+   adsurl = {http://adsabs.harvard.edu/abs/2017arXiv170809407C},
+  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
+}
+
+
 @ARTICLE{2017A&A...600A.125C,
    author = {{Cair{\'o}s}, L.~M. and {Gonz{\'a}lez-P{\'e}rez}, J.~N.},
     title = "{Integral field observations of the blue compact galaxy Haro14. Star formation and feedback in dwarf galaxies}",