The Carina star-forming region is one of the largest in the Galaxy, and its massive star population is still being unveiled. The large number of stars combined with high, and highly variable, interstellar extinction makes it inherently difficult to find OB stars in this type of young region. We present the results of a spectroscopic campaign to study the massive star population of the Carina Nebula, with the primary goal to confirm or reject previously identified Carina OB star candidates. A total of 141 known O-and B-type stars and 94 candidates were observed, of which 73 candidates had a high enough signal-to-noise ratio to classify. We find 23 new OB stars within the Carina Nebula, a 32% confirmation rate. One of the new OB stars has blended spectra and is suspected to be a double-lined spectroscopic binary (SB2). We also reclassify the spectral types of the known OB stars and discover nine new SB2s among this population. Finally, we discuss the spatial distribution of these new OB stars relative to known structures in the Carina NSebula. Subject headings: stars -massive -binaries: spectroscopic -open clusters and associations: individual (Carina)

The Carina Nebula is an active star forming region in the southern sky that is of particular interest due to the presence of a large number of massive stars in a wide array of evolutionary stages. Here we present the results of the spectroscopic analysis of 82 B-type stars and 33 O-type stars that were observed in 2013 and 2014. For 82 B-type stars without line blending, we fit model spectra from the Tlusty BSTAR2006 grid to the observed profiles of Hγ and He λλ 4026, 4388, and 4471 to measure the effective temperatures, surface gravities, and projected rotational velocities. We also measure the masses, ages, radii, bolometric luminosities, and distances of these stars. From the radial velocities measured in our sample, we find 31 single lined spectroscopic binary candidates. We find a high dispersion of radial velocities among our sample stars, and we argue that the Carina Nebula stellar population has not yet relaxed and become virialized. the mass, radius, and age. We also compare our results with any shared stars in past studies. Section 4 discusses the radial velocities and distances of the stars in our sample. OBSERVATIONSObservations of the stars were made at the Anglo-Australian Telescope (AAT) over the course of two runs in March 2013 and April 2014. The observations of these stars are described in greater detail by Alexander et al. (2016). We chose two different wavelength regions, 3925-4210Å (2013) and 4235-4510Å (2014), to cover many useful H and He lines for analysis. As the target spectra were vertically stacked on the imaging plane, distortions in the imaging plane meant that the exact spectral coverage varied among the targets and sky spectra. During our first day of observations in 2014, we used a slightly different range (4200-4475Å) for some of our exposures, but we found that this omitted the He I λ4471 line for some of our targets due to variable dispersion across the chip.The raw spectra were reduced using the dohydra package of IRAF and a custom IDL code for sky subtraction to account for the changing wavelength coverage across the CCD. Due to the variable dusty nature of the Carina Nebula, sometimes the average sky spectrum is too strong or too weak in comparison to our targets, which results in contamination of the Balmer line cores for some of our stars.Bright stars in our 2013 data generally have a signal-to-noise ratio (S/N) of 50-120, while the faint stars have a S/N of 30-70. The bright stars in our 2014 data have a S/N of 100-200, while the faint stars have a S/N of 120-210. The signal-to-noise of our 2013 data was low because our observing time was cut short due to wildfires in the area. We used two different fiber configurations for the bright versus the faint stars and observed them with different exposure times, which is how we achieved marginally better S/N for the fainter stars. Our measurements of S/N for each star are listed in Table 1.

The field of asteroseismology has enjoyed a large swath of data coming from recent missions (e.g., CoRoT, Kepler, K2 ). This wealth of new data has allowed the field to expand beyond the previous limitation of a few extremely bright and evolved stars. Asteroseismology relies on accurate surface measurements for boundary conditions, but the predicted physical parameters in the Kepler Input Catalog (KIC) are unreliable for hot stars. We present stellar parameters of 25 candidate pulsating B star candidates in the Kepler field. We use blue optical spectra to measure the projected rotational velocity (V sin i), effective temperature (T eff ), and surface gravity (log g) using TLUSTY and Kurucz ATLAS9 model atmospheres. We find a large discrepancy between our spectroscopically derived parameters and those derived from photometry in the KIC and Gaia Data Release 2 (DR2). Using spectral energy distributions, we also measure the radii of these stars and later calculate the luminosities and masses. We find the extinctions (A V ) of these stars to be consistent with zero, which is expected for stars of high Galactic latitude.