# Variability of young stellar objects in the star-forming region Pelican Nebula

## TL;DR

This study conducted extensive optical monitoring of the Pelican Nebula, identifying and classifying 95 variable stars, mainly pre-main-sequence stars, and analyzing their variability characteristics and physical properties.

## Contribution

It provides a detailed catalog of variable stars in the Pelican Nebula, including classifications, periods, and amplitudes, with insights into their variability behavior and physical parameters.

## Key findings

- 95 variable stars identified and classified.
- Classical T Tauri stars show larger amplitude variability.
- No correlation between variability amplitude/period and stellar mass or age.

## Abstract

We observed a field of $16'\times 16'$ in the star-forming region Pelican Nebula (IC 5070) at $BVRI$ wavelengths for 90 nights spread over one year in 2012-2013. More than 250 epochs in $VRI$-bands are used to identify and classify variables up to $V\sim 21$~mag. We present a catalogue of optical time-series photometry with periods, mean-magnitudes and classifications for 95 variable stars including 67 pre-main-sequence variables towards star-forming region IC 5070. The pre-main-sequence variables are further classified as candidate classical T Tauri and weak-line T Tauri stars based on their light curve variations and the locations on the color-color and color-magnitude diagrams using optical and infrared data together with Gaia DR2 astrometry. Classical T Tauri stars display variability amplitudes up to three times the maximum fluctuation in disk-free weak-line T Tauri stars, which show strong periodic variations. Short-term variability is missed in our photometry within single nights. Several classical T Tauri stars display long-lasting ($\geq 10$ days) single or multiple fading and brightening events up to a couple of magnitudes at optical wavelengths. The typical mass and age of the pre-main-sequence variables from the isochrone-fitting and spectral energy distributions are estimated to be $\le 1~M_\odot$ and $\sim 2$ Myr, respectively. We do not find any correlation between the optical amplitudes or periods with the physical parameters (mass and age) of pre-main-sequence stars.