Hubble Heritage 2.0
High quality images from Hubble have been the sine qua non in sustaining public support for the mission and astronomy in general. The Hubble Heritage project has been a key source of this imagery through a combination of archival and new images obtained over a decade. The success of Hubble's outreach efforts have spawned many imitators and it is essential for Hubble to invest a small fraction of time in maintaining our leadership in this area. With this proposal we seek to continue and refresh the Hubble Heritage project. We have focused on compelling targets that show off the capabilities of our reinvigorated observatory with an eye to new methods of image display and dissemination that will keep Hubble an iconic element of our culture.
Arp 273 emerged as our top candidate interacting galaxy pair after a search of the Arp catalog (Fig. 1) and we consider it to be of sufficient quality to serve as a potential 21st anniversary release image. The aesthetic appeal of this galaxy pair arises from the dynamic interaction of delicately detailed spiral arms. We propose to observe this target with a single WFC3 pointing in three filters for a total of 8 orbits (2 orbits per dither position). We will take advantage of the blue sensitivity of WFC3 to use a minimal filter set that highlights the blue star-forming regions in the near-UV and captures redshifted Hα emission in the “red” broadband filter (obviating the need for a separate Hα exposure). We will observe with WFC3 UVIS and use the F390W, F475X, and F600LP filters. Each of the filters will be exposed over a four point dither pattern to remove fixed-pattern artifacts and to cover the chip gap.
Supernova remnant SNR 0509 has archival data (Fig. 2) that show it to be a magnificent and stunning example of an unusually symmetrical supernova shell. There is nothing comparable to this object in the current inventory of Hubble imagery. The field of view in figure 2 is approximately one quadrant of the ACS. We will supplement this archival data with relatively short broad-band (F438W, F606W, and F814W) exposures with ACS to obtain star colors. We will use a 1-detector subarray to avoid serial buffer dumps. The existing Hα data will be layered in as a luminance layer (i.e. black and white). The result will be a striking combination of a colorful starfield with a mostly desaturated luminous shell (some color will be imparted from the broad band filters). HST data can be supplemented, as needed, with existing Chandra images of this SNR.
The Herbig Haro jet, HH 110, is a morphologically complex structure with turbulent eddies that form an evocative image (Fig. 3). We propose to supplement two epochs of archival Hα data with visible and IR broad band imaging to bring out stellar colors and penetrate ambient dust. We propose two orbits to obtain F438W, F814W, F110W, and F160W. Both of the IR filters include emission from H and Fe. All observations will be fully dithered to cover the chip gap. The two existing epochs from 02/2004 (4920 s total integration) and 11/2005 (2176 s) show small but detectable changes in the jet, allowing for an additional educational component to an image release. Jet motion introduces a possible complication for new imaging. However, by layering the archival data as a luminance layer and contolling the relative levels of the new and archival data we can avoid unnatural artifacts.
Hubble’s Variable 1 is arguably one of the most important stars in the history of modern astronomy. In the well-known plate of M31 annotated by Edwin Hubble, what he originally identified as a nova has the identifying letter N crossed out and replaced with VAR! The discovery of a 21st magnitude Cepheid placed the “Great Andromeda Nebula” at a then unprecedentedly remote distance. Surprisingly, this keystone object has sunk into relative obscurity and has never been observed by the telescope named for its discoverer. We propose to remedy that oversight with a 4-orbit observation to capture the star and its neighboring galactic field in deep broadband UVIS (2 orbits, F475X and F600LP) and IR (1 orbit, F110W) imaging. We will observe a second visit in F600LP at a different phase of the Cepheid lightcurve to be able to show variability. While the image will be of a non-descript star in a relatively ordinary starfield, we believe that the historical significance of this object and the fascinating stories attached to it (e.g. a copy of the plate was flown on the SM4 mission) justify this effort. For this target we will partner with David Soderblom, who proposed this idea, and several other colleagues. We have also contacted the Mt. Wilson 100-inch to inquire about a possible collaboration that would include new imaging from this historic telescope and access to other historic artifacts (although availability of instrumentation may limit their participation).
S106 is a well-known nearby HII region with a bipolar architecture. Bally and colleagues obtained Hα imagery of this region with WFPC2. We are proposing to obtain data in two additional emission lines, O [III] and Paschen β to allow rendering this target in color. We will also obtain additional Hα data to allow for alignment with archival data. Because the lobes have different extinction, the addition of the longer wavelength hydrogen line will allow for a dramatic color visualization of the dust penetrating ability at infrared wavelengths on an extended source. Because the orientation of the target is known and also because of the detailed scalloping of the lobes, this target will be outstanding in 3D. A diagonal orientation fits both lobes into a single WFC3 UVIS frame. In the IR we will dither to cover the same area. Integration times can be estimated from existing data. We propose 2 orbits of UVIS observation and 1 orbit of IR for a total of 3 orbits for this target.
We have run test visits through APT to confirm the schedulability of these observations. As always, we design our phase 2’s to minimize the impact on the GO schedule. We do this by breaking long visits into shorter, more schedulable visits and by minimizing constraints. We will work with the PC to ensure we meet this goal.
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