tokens: galaxies. These objects were used to draw conclusions about the AGN population that would be missed in optical and X-ray surveys. Of the 30 AGN candidates using the Jarrett et al. ( 2011 ) selection box and presented in Satyapal et al. ( 2014 ), only one object is in the mass and redshift range probed by our analysis here (the others are either at higher masses or higher redshifts), and it is found in our sample of star-forming dwarfs in the Jarrett et al. ( 2011 ) box (NSA ID 93798). Secrest et al. ( 2015 ) measured an X-ray luminosity from XMM-Newton observations (extracted with a ∼15′′ aperture) of L 2–10 keV = 2. 4 × 10 40 erg s −1 for this object, and claim that the W1 − W2 color is strongly indicative of AGN activity. While this object is indeed in the Jarrett et al. ( 2011 ) selection box, given the median uncertainties on the WISE photometry, its infrared colors are consistent with this object potentially being scattered from the primary locus of star-forming galaxies and it does not have a strong power law to longer infrared wavelengths as expected for an AGN. Sartori et al. ( 2015 ) presented a sample of 83 objects with photometry placing them in the Jarrett et al. ( 2011 ) selection box, using data from the older WISE All-sky data release. These authors only required S/N > 2 for detections in the W1 , W2 , and W3 photometric bands. We cross-matched against the more up-to-date AllWISE selection, and using a S/N cut of 3.0, we find that only 34 objects (∼41%) continue to fall inside the Jarrett et al. selection box. 9 9 All 83 of the objects in the Sartori et al. ( 2015 ) sample have updated AllWISE W1 and W2 photometry with S/N > 3.0, but 26 of the objects have W3 photometry with S/N 3, only 10 of which have 2 S/N 3. Of these 34 objects, only 15 are in our parent sample of dwarf galaxies. The remaining 19 objects are either not in the NSA because their redshifts are greater than 0.055, or are in the NSA but not classified as dwarf galaxies by our mass criterion. Looking closer at these 15 dwarf galaxies, 10 are found in Table 1 (NSA IDs 4610, 6205, 10311, 53934, 57649, 93798, 109919, 117162, 118025, and 118523), 4 of the 15 are BPT-selected AGNs or composite galaxies (NSA IDs 10779, 79874, 124050, and 125318), and one is the previously discussed quasar contaminant (NSA ID 110100). One object that was listed as a Stern et al. ( 2012 ) candidate but not a Jarrett et al. ( 2011 ) candidate in Sartori et al. ( 2015 ) moved into the Jarrett et al. ( 2011 ) selection box with the updated AllWISE photometry (NSA ID 98135), and one object we have listed in Table 1 does not appear in Sartori et al. ( 2015 ) (NSA ID 151888). 3.5. The Feasibility of Detecting Supermassive Black Holes in Dwarf Galaxies with WISE Finding evidence for AGNs in dwarf galaxies is challenging as AGNs at a given accretion rate have lower bolometric luminosities due to the smaller masses of the central black holes, making them harder to observe above the emission due
ner_tags: O O O O O O O O O O O O O O O O O B-Wavelength O B-Wavelength O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O B-CelestialObject I-CelestialObject I-CelestialObject B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O B-Wavelength O O B-Telescope O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O B-Wavelength O B-Wavelength O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O B-Telescope O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O B-Dataset I-Dataset I-Dataset I-Dataset O O O O B-Formula I-Formula I-Formula O O O O B-Wavelength O B-Wavelength O O B-Wavelength O O O O O O O O B-Survey O O O O O O O O O O O O O O O O O O O O B-CelestialRegion I-CelestialRegion I-CelestialRegion I-CelestialRegion I-CelestialRegion O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O B-Survey B-Wavelength O B-Wavelength O O B-Formula I-Formula I-Formula O O O O O O B-Wavelength O O B-Formula I-Formula O O O O O B-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O B-Dataset O O O O O O O O O O O B-Dataset O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject B-CelestialObject B-CelestialObject B-CelestialObject B-CelestialObject B-CelestialObject B-CelestialObject B-CelestialObject O B-CelestialObject O O O O O O O O O O B-CelestialObject I-CelestialObject I-CelestialObject B-CelestialObject B-CelestialObject O B-CelestialObject O O O O O O O O B-CelestialObject I-CelestialObject I-CelestialObject O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O B-Survey O B-CelestialObject I-CelestialObject I-CelestialObject O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation B-CelestialObject I-CelestialObject I-CelestialObject O O O O O O O O O O O O B-Telescope O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O