==========================================================================
II/362 i-band variability of YSOs (Sergison+, 2020)
The following files can be converted to FITS (extension .fit or fit.gz)
stars.dat tablea.dat tableb.dat tablec.dat tabled.dat
==========================================================================
Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=II/362
==========================================================================
drwxr-xr-x 351 cats archive 8192 Mar 25 10:13 [Up]
drwxr-xr-x 3 cats archive 4096 Jan 12 2023 [TAR file]
-rw-r--r-- 1 cats archive 504 Dec 19 2022 .message
-r--r--r-- 1 cats archive 10539 Jan 9 2020 ReadMe
-rw-r--r-- 1 cats archive 1005 Jan 10 2020 +footg5.gif
-rw-r--r-- 1 cats archive 2965 Jan 10 2020 +footg8.gif
-r--r--r-- 1 cats archive 408389 Nov 7 2019 stars.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 493166377 Nov 6 2019 tablea.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 2853922 Nov 6 2019 tableb.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 7033679 Nov 6 2019 tablec.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 2906562 Nov 6 2019 tabled.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe :II/362 i-band variability of YSOs (Sergison+, 2020)
================================================================================
Characterising the i-band variability of YSOs over six orders of magnitude
in timescale.
Sergison D.J., Naylor T., Littlefair S.P., Bell C.P.M., Williams C.D.H.
<Mon. Not. R. Astron. Soc. 491, 5035 (2020)>
=2020MNRAS.491.5035S
=2020yCat.2362....0S
================================================================================
ADC_Keywords: Clusters, open ; YSOs ; Photometry, SDSS
Keywords: open clusters and associations: individual: Cep OB3b -
stars: formation - stars: pre-main-sequence - stars: rotation -
stars: variables: T Tauri - accretion
Abstract:
We present an i-band photometric study of over 800 young stellar
objects in the OB association Cep OB3b, which samples timescales from
1 minute to ten years. Using structure functions we show that on all
timescales (tau) there is a monotonic decrease in variability from
Class I to Class II through the transition disc (TD) systems to Class
III, i.e. the more evolved systems are less variable. The Class Is
show an approximately power-law increase (tau^0.8^) in variability from
timescales of a few minutes to ten years. The Class II, TDs and Class
III systems show a qualitatively different behaviour with most showing
a power-law increase in variability to a timescale corresponding to
the rotational period of the star, with little additional variability
beyond that timescale. However, about a third of the Class IIs show
lower overall variability, but their variability is still increasing
at 10 years. This behaviour can be explained if all Class IIs have two
primary components to their variability. The first is an underlying
roughly power-law variability spectrum, which evidence from the
infrared suggests is driven by accretion rate changes. The second
component is an approximately sinusoidal and results from the rotation
of the star. We suggest that the systems with dominant
longer-timescale variability have a smaller rotational modulation
either because they are seen at low inclinations or have more complex
magnetic field geometries. We derive a new way of calculating
structure functions for large simulated datasets (the "fast
structure function"), based on fast Fourier transforms.
Description:
We give tables of the i-band lightcurves of stars in the region, along
with structure functions and lightcurve statistics.