Cloud limit was raised to 70%. This should allow some backlogged requests to get through bouncy castle.
The camera is hung in a state that requires a power cycling.
Camera fails to execute a software reset
The camera returns the error “failure in reset”
The leach controller window shows highly incorrect values in gain (e.g., -4095), amp, heat, bouncy castle etc.
Cycle the power on the camera on site (cannot be done remotely). It is unclear where this problem stems from.
A 30-second exposure of the HII region, M42 (the Orion Nebula) taken through the RCT’s Hα filter. The full-field image is nearly 10 arcminutes square with North up and East to the left. Major features such as the Dark Bay (upper left), the Bar and the Trapezium stars (center) are clearly visible. The zoomed image presents a more detailed view of the inner region of the nebula. Stars fainter than 16th magnitude jumping castle are visible near the Trapezium. Emission features such as ionized knots and shock fronts are clearly visible.
Blazars and other galaxies with active nuclei have been a significant focus of RCT research, as queue scheduled observations have facilitated monitoring the variable energy output of these sources. These data are then combined with observations by collaborators at other wavelengths, providing a clearer picture of the behavior of the material in the relativistic jet and central engine.
Composite light curve for the well-known AGN II ZW 229.015, showing data from the RCT (red), Barth et al. (2011, yellow), and the Kepler satellite. RCT image of II ZW 229.015 to the right taken on 06/05/2013.
The complete data set analyzed by Williams and Carini (2013) yields a break in the slope of the Power Spectrum Density (PSD) which implies a central black hole mass of 12 million solar masses, as shown in the above graph.
Comet P/2013 EV9 observed with the RCT on April 30, 2013. 54 120-second exposures were stacked to produce this composite. Click for sharper image.
Minor solar system bodies are a routine part of RCT observations, and results have appeared in numerous Minor Planet Circulars. Motions up to 3.5”/min. are readily tracked.
In this post we summarize continuing efforts to monitor the strange behavior of M33 V19 in B and V using the RCT. With the ability of a robotic telescope to do time series observations, we hope to gain a better understanding of this ‘previously-a-Cepheid’ object’s unprecedented evolutionary behavior.
In 1926, Hubble determined the distance to M33 using 35 Cepheids he discovered, one of which was his Variable 19, with a period of 54.7 days, an amplitude in B of 1.1 mag, and a mean B magnitude of about 19.6. DIRECT project observations in 1996-7 with the 1.2m Whipple and 1.3m MDM telescopes and RCT observations, together with other data, clearly show that the star’s amplitude has diminished to less than 0.1 mag, while the star’s mean
brightness increased substantially.
Below is a another figure showing photometry of a fainter nearby Cepheid from both the RCT and the DIRECT project, showing that photometric quality is comparable.
RCT observations of SN2011fe in M101 show the power of queue scheduled observations. The SN is circled in the above image. Diagram from Strolger et al. (2014, in press). RCT observations are shown as solid circles with error bars, while AAVSO observations are shown for comparison. Click for a sharper view of the figure below.