PTF10nvg: An Outbursting Class I Protostar in the Pelican/North American Nebula

TL;DR

PTF10nvg is a newly observed outbursting Class I protostar in the North American Nebula, showing significant brightening and rich emission lines indicative of increased accretion and outflow activity.

Contribution

This paper reports the discovery and detailed spectroscopic analysis of PTF10nvg's outburst, revealing its nature as an active, accreting protostar with dense circumstellar material.

Findings

Brightened by over 5 magnitudes in optical and infrared bands.

Displays blueshifted emission lines indicating outflows.

Shows dense, warm circumstellar material with emission TiO/VO bands.

Abstract

During a synoptic survey of the North American Nebula region, the Palomar Transient Factory (PTF) detected an optical outburst (dubbed PTF10nvg) associated with the previously unstudied flat or rising spectrum infrared source IRAS 20496+4354. The PTF R-band light curve reveals that PTF10nvg brightened by more than 5 mag during the current outburst, rising to a peak magnitude of R~13.5 in 2010 Sep. Follow-up observations indicate PTF10nvg has undergone a similar ~5 mag brightening in the K band, and possesses a rich emission-line spectrum, including numerous lines commonly assumed to trace mass accretion and outflows. Many of these lines are blueshifted by ~175 km/s from the North American Nebula's rest velocity, suggesting that PTF10nvg is driving an outflow. Optical spectra of PTF10nvg show several TiO/VO bandheads fully in emission, indicating the presence of an unusual amount of dense (> 10^10 cm^-3), warm (1500-4000 K) circumstellar material. Near-infrared spectra of PTF10nvg appear quite similar to a spectrum of McNeil's Nebula/V1647 Ori, a young star which has undergone several brightenings in recent decades, and 06297+1021W, a Class I protostar with a similarly rich near--infrared emission line spectrum. While further monitoring is required to fully understand this event, we conclude that the brightening of PTF10nvg is indicative of enhanced accretion and outflow in this Class-I-type protostellar object, similar to the behavior of V1647 Ori in 2004-2005.