0Assigned ID: 1004
----- Attempting Submission 1 (Sat Feb 25 00:34:27 GMT 2012) -----
HST Phase I Proposal 1004 (phase1-GO.pdf.apt) successfully submitted.
----- Attempting Submission 2 (Sat Feb 25 00:49:53 GMT 2012) -----Added visit 59 as a repeat of failed visit 09.118520055----- Attempting Submission 1 (Tue Jul 10 20:35:32 GMT 2012) -----
----- Attempting Submission 2 (Sat Feb 16 00:01:37 GMT 2013) -----
----- Attempting Submission 3 (Fri Apr 05 02:08:23 GMT 2013) -----Visit 59 has been created as a repeat and will be processed after submission.Local Turbulent Disks: analogs of high-redshift vigorously star-forming disks and laboratories for galaxy assembly?Kinematical investigations at redshifts 1<z<3 with Keck and VLT have revealed that star-forming high-redshift galaxies exhibit very high internal velocity dispersions. Dynamical data collected with integral field spectrographs (IFS) suggest that the level of rotational support in these systems follows a trend in mass, with compact dispersion-dominated Lyman Break Galaxies at lower stelar masses and large dynamically unstable turbulent disks at stellar masses larger than 10^10 solar masses. The high velocity dispersion of these young disks results in a large characteristic scale for star-forming clusters thereby also explaining their 'clump cluster' morphology. Galaxies like these were thought to be absent from the local Universe. As part of a IFS campaign to observe the most H-alpha luminous galaxies in SDSS, we have discovered a sample of very rare objects seemingly identical to these high-z turbulent disks. In this proposal we seek imaging in H-alpha of thirteen local disk galaxies in our sample, using the ACS tunable-wavelength ramp filters. Our goal is to measure the size distribution of the star-forming complexes in these objects, with ten times the typical physical resolution of HST observations of high-z galaxies, in order to test the idea that they are indeed dynamically unstable turbulent disks caught in the process of formation. In synergy with existing high resolution HST imaging of the local analogs of low-mass dispersion-dominated galaxies at high redshift (Lyman Break Analogs), our proposed observations of the local counterparts to large turbulent disks at high redshift will help to paint a complete picture of local analogs of high-z star-forming galaxies.Sample selection:
Our ACS targets have been selected from the DYNAMO (Dynamics of Newly Assembled Massive Objects) sample that has been observed using the AAT SPIRAL and Stromlo 2.3m WiFeS integral field spectrographs. DYNAMO targets are the most extreme Halpha-luminous galaxies in the entire SDSS (excluding AGN) with star formation rates (SFRs) that match the high SFRs of dynamically unstable star-forming disks being studied at high redshift. Redshift windows (within 0.05<z<0.15 range) were chosen to avoid night sky absorption and emission contamination. Our surprising discovery was that all DYNAMO sample galaxies at high Halpha luminosities have high internal velocity dispersions of up to sigma_m=100 km/s. While some of high sigma_m DYNAMO objects have merger-like large-scale kinematics, at least half the sample have kinematics very similar to high-z disks suggesting we have indeed discovered local turbulent disks.
Since almost all local and high-z surveys aimed to study spatially resolved dynamical and structural properties of star-forming galaxies have been focused on the rest-frame Halpha observations, we will use narrow-band Halpha imaging with FR716N and FR782N ACS ramp filters to study the morphology of star-forming clumps at z~0.1 and compare it to the structural properties of high-z star-forming systems. In addition, the monochromatic field of view of the ACS ramp filters (equal to or larger than 25" x 60") is ideal for our purposes, since galaxies in our sample are typically 10 to 15" in size.
All DYNAMO targets in our ACS sample of ten high velocity dispersion (sigma_m> 50 km/s) galaxies with 0.05 < z < 0.15 are objects with clear evidence for regular disk rotational motions (v_shear/sigma_m>1). All these objects have Halpha luminosity L(Halpha) > 10^41.9 erg/s. This luminosity cut was chosen to match the typical luminosities of the high-z populations of star-forming galaxies reported in Forster Schreiber et al. (2009), Law et al. (2009), Epinat et al. (2009) and Lemoine-Busserolle & Lamareille (2010). The sample covers a factor of ~10 in stellar mass (10^10.1 to 10^10.9 Msun), matching the massive turbulent disks in the z~2 SINS sample (Forster Schreiber et al. 2009). The dust extinctions (derived from Halpha/Hbeta) are also comparable with A(Halpha) ~ 0.8 mag found at high redshift.
The remaining three objects in our control sample were chosen from the subset of lower luminosity DYNAMO galaxies (Halpha < 10^41.9 erg/s) with low velocity dispersion (sigma_m < 50 km/s) and showing clear evidence for rotation. Our purpose in imaging a control sample is to make sure we have a sample of well-understood objects imaged through the ramp filters, since these filters have not been used very often on z ~0.1 galaxies with ACS.
Visit set-up, integration times, and the aperture selection:
Our central goal is to measure the sizes of HII regions in the selected sample using narrow-band filter FR716N or FR782N. In addition, short integration off-band images in FR647M will be used for continuum subtraction. Each visit will consist of four exposures: one pair in a narrow-band and another pair in the broad-band ramp filter. In order to maximize the exposure time, narrow-band imaging in FR716N and FR782N filters consists of two exposures corresponding to two distinct pattern positions (ACS-WFC-DITHER-LINE) that will be used for cosmic ray and hot pixel rejection. Within chosen dither pattern point spacing of ~0.7" (~10 pixels) has been selected to ensure that the observed object is within the quasi-monochromatic patch at each position. Two shorter exposures in the medium-band FR647M filter mimic the dithering pattern used with the narrow-band filter, since the last exposure of each visit (340 to 355s in FR647M) is taken with an offset (x=0.07", y=0.72"). This set-up allows us to minimize the time lost on the overheads for exposures shorter than 340s. The set-up used for the FR647M-FR782N filters combination (visits 01, 03, 08 and 10) features shorter exposure times because two filters cannot be placed on the same WFC chip (and thus require a guide star acquisition when exchanging fitters, see below).
The choice of narrow-band filter is governed by the redshift of each object in our sample, since it will change the observed wavelength of Halpha line. Majority of galaxies in the sample (9/13) are at redshift z<0.14 and their HII regions will be observed using FR716N, which covers the same aperture as the broad-band filter FR647M used for continuum subtraction (WFC1-IRAMP aperture). This combination of filters allows for the maximum exposure times: ~1400s in FR716N and ~700s in FR647M. Based on the ACS ETC results we expect SNR > 5 in an aperture with the radius of 0.1" for both narrow- and broad-band filters for the least luminous galaxy in our sample, ELfluxLz_4 at redshift z=0.069 and with Halpha luminosity of log(L(Halpha)[ergs/s])=41.36. Another four objects in our sample lie at redshift z~0.15 and their HII regions will be spatially mapped using the FR782N filter. Since FR782N and FR647M filters do not share the same aperture, exposure times for these targets will be shorter to allow for the guide star acquisition after the exchange of filters: ~710s and ~460s in FR782N and FR647M, respectively. However, these four objects are the most luminous targets in our sample with Halpha luminosities of log(L(Halpha)[ergs/s])>42.1 and thus we will still be able to achieve SNR > 5 in an aperture with the radius of 0.1" for both filters.
Although ramp filter apertures cover only a fraction of the full WFC field of view (FoV), we will use full FoV instead of subarrays. Our decision is motivated by the fact that the background in ramp filter images is usually extremely low, producing high charge transfer efficiency (CTE) losses that can compromise the quality of obtained images. For full FoV frames a pixel-based CTE correction is performed as part of the new ACS calibration pipeline (CALACS). Furthermore, full FoV frames can also be corrected for bias striping.UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE12falsefalse0.00.0falsefalsefalseSUPPORTEDGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^42.37 ergs/sGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^42.58 ergs/sGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^42.16 ergs/sGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^42.36 ergs/sGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^42.10 ergs/sGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^42.23 ergs/sGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^41.93 ergs/sGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^42.26 ergs/sGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^42.05 ergs/sGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^42.52 ergs/sGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^41.36 ergs/sGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^41.76 ergs/sGALAXYDISKSTAR FORMING REGIONJ2000J2000Halpha luminosity = 10^41.94 ergs/sACS/WFCRampFilterNoNoFR782NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR782NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR782NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR716NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR716NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR782NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR716NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR782NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR716NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR782NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR716NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR716NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR716NACS/WFCRampFilterNoNoFR647MPOS-TARGDITHER0.693LINEfalsefalse285.28ACS-WFC-DITHER-LINE1falseThe scheduling data was generated by CASM 21.0.CASM was run in Phase II mode.1364061460000112.23660030418239(Tic-Visit
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:si-vis-utilization 2682
:al-overhead-at-end 0
:internal-dur-at-end 347
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3015
:pcs-gap 0
)true10