HERE is the cover photo (DCT).
Caption: Architectural rendering of the Discovery Channel Telescope.
Use the picture of Merav and her Old View/New View image from the .docx file that she sent us.
Caption for Merav: Professor Merav Opher speaking during the April 28th NASA TV live broadcast on the impact and results from the Voyager mission.
Caption for the image: Old and new views of the heliosheath. The red and blue spirals are the gracefully curving magnetic field lines of the orthodox models. New data from Voyager add a magnetic froth (highlighted by the insert) to the mix. Image credit: NASA (based on a model constructed by Professor Opher and her colleagues).
Also use the picture of Ken Janes from the BU website.
Caption: Professor Emeritus Kenneth Janes.
HERE are two pictures for Liz's research. Ideally, they should go side
by side in the text.
Caption: Left: Residual X-ray image (0.3-2.0 keV band) of the central 240 kpc radius region of galaxy cluster A2052, after a model has been subtracted. An excess "sloshing spiral" is revealed, and is related to an off-axis cluster or sub-cluster merger likely billions of years in the past. Right: Temperature map of galaxy cluster A2052 with the contours of the sloshing spiral superposed. The scale bar shows T in keV. The spiral feature is significantly cooler than its surroundings.
HERE is a picture for Dan's research.
Caption: Plot of polarization percentage versus galactic longitude. The polarization is averaged across the Mimir field of view for 400+ fields. The data reveal a a modulation that is most likely caused by changing magnetic field properties in, and between, spiral arms in our galactic disk. Mimir's polarimetric sensitivity extends to distances and depths into the galactic dust that no other instrument has been able to see.
HERE is the first picture for Jackson's research.
Caption: Views of the Nessie Nebula. Top panel: Nessie as seen in the infrared at 3.6 microns (blue), 8.0 microns (green), and 24 microns (red). Second panel: the same with integrated HNC (1-0) contours, showing the excellent correspondence between HNC (1-0) emission and 8 micron extinction. Third panel: cyan crosses showing the positions of cores on the HNC (1-0) integrated intensity map. Bottom panel: the velocity field (first moment) of HNC (1-0). All the emission is within 4 km/s, demonstrating that the filament is a single coherent object.
HERE is the second picture for Jackson's research.
Caption: Near-infrared (K-band) image of the object known as G034.43+00.24 MM3 taken with the NIRC2 campera on the 10-m Keck telescope using adaptive optics. The image shows high-resolution details of the outflows in the central cluster and a previously undetectable population of distributed low-mass protostars identified by protostellar outflows around very red point sources.
HERE is the third picture for Jackson's research.
Caption: The distribution of MALT90 HNC source velocities from Year 1 (red histogram) overlaid on the 12CO spectrum from the CfA-Columbia CO survey, averaged over the same region (black histogram). The MALT90 sources show a more narrowly-peaked distribution, indicating that the regions of high-mass star formation are tightly confined to spiral arms.
HERE are two pictures for the blazar
group's reasearch. Ideally,they should go side-by-side in the text.
Caption: Shown on the left is the brightness of the quasar 3C 454.3 as a function of time at gamma-ray, X-ray, visible red, and microwave (millimeter) wavelengths. The peaks in 2008-09 were considered to be "major" until they were dwarfed by the "mega-outburst" that occured in late 2010. The upward blue arrows at the bottom show the times when a bright "blob" passed through the stationary bright region called the "core," which lies 10-50 light-years from the black hole. Shown on the right are a time sequence of images of the "blob" and "core", where the blob is located to the left of the core. The blazar group interprets these events as the result of turbulent, high-energy, magnetized plasma flowing across one or more standing shocks that compress and heat the plasma.
HERE is the first picture for Andrew's research.
Caption: The line of sight visual extinction to more than 50,000 M dwarfs as a function of Galactic height (Z) and Galactocentric radius (R). The azimuthal direction has been compressed in this figure.
HERE is the second picture for Andrew's research.
Caption: Sloan Digital Sky Survey gri composite images of ~3000 images from Professor West's spectroscopic M dwarf sample. The images were put together to mimic the logo of the "Cool Stars 16" conference logo (credit L. Walkowicz) that took place in Seattle, WA in August 2010.
HERE is a picture for undergradute
Caption: AS102 students with the Mimir instrument on the Perkins Telescope.
HERE is another picture for undergradute
Caption: AS 102 students with Dean Sapiro in the Perkins Telescope control room, during observations with the Mimir instrument to conduct the research projects for the class.
HERE is another picture for undergradute
Caption: AS102 students in the Phoenix Airport. One group of 6 students was headed home to Boston after completing their observations. The other group of 6 students was just arriving and headed up to Flagstaff to conduct their observations.
HERE is a picture of Ned and HERE is a picture of Josh. Ideally, they should go side by side in the text.
Caption: Graduate students Josh Wing (left) and Net Douglass (right) presenting
their poster papers at the May 2011 meeting of the American Astronomical Society
in Boston, MA.
HERE is a picture of the Perkins.
Caption: The 1.8m Perkins Telescope.
HERE is a .docx file that contains 3 pictures
relating to PRISM. We will use the 2nd and 3rd pictures only.
Caption for the 2nd picture in the .docx file: The new science array for PRISM installed in the dewar.
Caption for the 3rd picture in the .docx file: First light image from PRISM with the new detector installed.