%0 Generic %1 krishnarao2016study %A Krishnarao, Dhanesh %A Haffner, L. Matthew %A Benjamin, Robert A. %D 2016 %K ionized medium milky warm way %T A Study of the Warm Ionized Medium Throughout the Sagittarius-Carina Arm %U http://arxiv.org/abs/1610.08785 %X We present velocity-channel maps and analysis of the warm ionized medium (WIM) throughout the Sagittarius- Carina arm at Galactic longitudes 20 < l < 52 and 282 < l < 332. Using Wisconsin H-Alpha Mapper observations of H-alpha and S II 6716 emission, the structure of the WIM along a longitude-velocity track corresponding to CO emission in the plane is isolated. Exponential scale heights of electron density squared (or emission measure) are determined using H-alpha emission above (below) the midplane to be 330 plus/minus 80 pc (550 plus/minus 230 pc) along the near Sagittarius arm, 300 plus/minus 100 pc (250 plus/minus 30 pc) along the near Carina arm, and > 1000 pc along the far Carina arm. Physical conditions of the ionized gas are analyzed using the S II/H-alpha line ratio, which more closely traces H-alpha intensity than height above the plane, z, suggesting a stronger relationship with the in-situ electron density. We interpret this result as further evidence for the majority of the observed diffuse emission originating from in-situ ionized gas as opposed to scattered light from classical H II regions in the plane.

@misc{krishnarao2016study, abstract = {We present velocity-channel maps and analysis of the warm ionized medium (WIM) throughout the Sagittarius- Carina arm at Galactic longitudes 20 < l < 52 and 282 < l < 332. Using Wisconsin H-Alpha Mapper observations of H-alpha and [S II] 6716 emission, the structure of the WIM along a longitude-velocity track corresponding to CO emission in the plane is isolated. Exponential scale heights of electron density squared (or emission measure) are determined using H-alpha emission above (below) the midplane to be 330 plus/minus 80 pc (550 plus/minus 230 pc) along the near Sagittarius arm, 300 plus/minus 100 pc (250 plus/minus 30 pc) along the near Carina arm, and > 1000 pc along the far Carina arm. Physical conditions of the ionized gas are analyzed using the [S II]/H-alpha line ratio, which more closely traces H-alpha intensity than height above the plane, z, suggesting a stronger relationship with the in-situ electron density. We interpret this result as further evidence for the majority of the observed diffuse emission originating from in-situ ionized gas as opposed to scattered light from classical H II regions in the plane.}, added-at = {2016-10-28T09:28:22.000+0200}, author = {Krishnarao, Dhanesh and Haffner, L. Matthew and Benjamin, Robert A.}, biburl = {https://www.bibsonomy.org/bibtex/298f555e976faf6dc5391393ced334fc9/miki}, description = {[1610.08785] A Study of the Warm Ionized Medium Throughout the Sagittarius-Carina Arm}, interhash = {6b6e1fbd55a7d12efc1564fd4caed5ea}, intrahash = {98f555e976faf6dc5391393ced334fc9}, keywords = {ionized medium milky warm way}, note = {cite arxiv:1610.08785}, timestamp = {2016-10-28T09:28:22.000+0200}, title = {A Study of the Warm Ionized Medium Throughout the Sagittarius-Carina Arm}, url = {http://arxiv.org/abs/1610.08785}, year = 2016 }