The slides in this collection are all related and should be useful in preparing a presentation on SIM PlanetQuest. Note, however, that there is some redundancy in the collection to allow users to choose slides best suited to their needs. Taking the Measure of the Milky Way
The slides in this collection are all related and should be useful in preparing a presentation on SIM PlanetQuest. Note, however, that there is some redundancy in the collection to allow users to choose slides best suited to their needs.
Cover page from S. Majewski
Key Project proposal
You are here
SIM will test this model
Simulated ‘time-lapse’ photo of
30 galaxies closest to our Milky Way
(1-billion year exposure)
5% error in Mass
Taking Measure of the Milky Way Key Project will provide unique insight into the following key issues:
We will also independently:
‘Tidal tail’ simulation:
Dwarf galaxy in orbit around the Milky Way
(Sgr, Pal 5, Monoceros/Argus, TriAnd)
Leading Arm RVs “wrong”;
Prolate vs. Oblate ambiguity
SIM can determine if the visible light from quasars originates in hot gas around an accretion disk or from a relativistic plasma jet
SIM can detect the orbital motions of two merging black holes in the centers of massive galaxies
200,000 ly structure generated by jets in M87
What are the sizes and geometric relations between the components of the “core” region: jets, accretion disk, hot corona ?
Which components dominate the optical emission?
The structures we measure with SIM are either optical synchrotron emitters from particle populations distinct from the radio-synchrotron emitters, or thermal emitters from the hot corona or accretion disk.
Since we wrote our SIM proposal in 2000, Seyfert nuclei of NGC 4151 and NGC 1068 were detected by Keck Interferometer and VLTI, respectively, (Swain et al. 2003, ESO 2003).
Binary black holes may be ubiquitous in galactic centers, rather than rare, because mergers may stall out. Orbital motion of binary black holes is detectable with SIM, using astrometric reflex motion of their photocenter, just like we detect planets around stars.
Quasars in the range of V~ 15-17, but a few are brighter, such as 3C273
Historically, the most compact quasars are the most variable, so we need to ensure the ones we observe with SIM are consistently the brightest.
We have begun a monitoring program on the Palomar 60” telescope.
Discussions with European (and other) monitoring groups have begun (international conf. in April 2005)
Strong, non-coincidental agreement on source lists with GLAST mission (launch 2007) - brightest, most compact blazars are the ones they are most likely to detect