Top/Workshops/4th Science Workshop/QandA_MEMOs

#11:05  "Current Status of SWIMS and Expected Performance on Subaru
Telescope"   (30min)    K. Motohara (NAOJ)

(Masataka Imai-san)
minimum exposure time for bright objects? => 1.5 sec
Is observation of bright object possible ? => depends on science case you need, please contact individually.

(Kenneth Wong-san)
When the IFU becomes available?
=> Earliest S22B, with optimistic expect.

(Kimihiko Nakajima-san)
Do you plan to have a software for MOS mask design to avoid detector gaps, etc?
=> No software at the moment, but prepare information to design.

(Hanae Inami-san) 
When SWIMS goes to TAO? => from S23A
When IFU becomes available ? => probably only S22B, if the development goes well.
What is FoV of the IFU => 14.0"x5.2" on Subaru

[Comment] IFU should go through review and get approved to be served at open-use.

How we can choose SWIMS or MOIRCS? What is the merit of SWIMS?
=> MOIRCS will be hibernated during SWIMS operation.

#11:35  "PI Instrument Operation at Subaru Telescope" (10min)    Y. Koyama (NAOJ)
Is any delay for the deadline of CfP due to COVID-19?
=> delay
If SWIMS fails, is MOIRCS also provided under risk-share => no, MOIRCS will be provided stably.

#11:45  Q&A (15min)             
No question

#[Science Session 1] (Chair: Konishi)
#13:00  "SWIMS-18 survey and its pilot observations on Subaru" (20min)  T.
Kodama (Tohoku Univ.)

Halpha in clusters at z~0.9 : any plan for diffuse Halpha emission by
going deeper?
=> May be possible, but probably for TAO science, as 
it requires large amount of time.However, proposed z~0.9 is 
in the northern hemisphere and cannot be observed from TAO.

About redshift evolution of red sequence galaxies :
if the redshift evolution of red galaxy is flat, red fraction 
gets larger at higher-z as number of SF galaxy decreases at high-z?

What is the advantage against ZFOURGE?
=>FoV of ZFOURGE is ~300arcmin^2 in Ks

#13:20  "Search for protoclusters at z~4-5: plausible sites of the
formation of massive galaxies"  J. Toshikawa (Univ. Tokyo)
No question

#13:40  "Investigation of chemical enrichment in the early universe by
observing high-z quasars" (20min)       H. Sameshima (Univ. Tokyo)

Metallicity plane EW(MgII) vs EW(FeII): Mg/Fe and Fe/H from CLOUDY simulation
 There is a discrepancy between CLOUDY simulation and observations; any comments?
=>Need to check.

Already a lot of archive spectra of high-z QSOs, and using them, you can start now?
=> Probably yes.

#14:00 "SWIMS spectroscopy of HSC-NB emitters at z~1.47", Masao Hayashi (NAOJ)
Your proposal requires 6 masks in 2 nights, but we can use up to 4 masks per one observing run. Is it OK for your project? (Motohara-san)
—> I may change the strategy according to the instrumental limitation. 

#14:20 "Spectroscopy of dual quasars from HSC ", John Silverman (U Tokyo)
What is the wavelengths you need? (Motohara-san)
—>  We can choose QSOs at the redshifts matched with the SWIMS wavelength coverage. 

What is the required spatial resolution? (Motohara-san)
—> Typical separation of the dual cores is 0.6–0.4 arcsec. 
       Natural seeing conditions would be fine. Wider separation QSOs (~0.6 arcsec) are suitable for IFU obs. with TAO. 

J1614 seems to have the extended H-alpha emission connecting the core and host (bridge-like structure). Is this real? (Saito-san)
—> I need to check the data more carefully to conclude whether this structure is real or not. 

#15:00 “Characterization of Exoplanets by the Synergy of SWIMS and MuSCAT3", Mayuko Mori (U Tokyo)
What is a typical magnitude of your targets? (Motohara-san)
—> 11-18 mag for TESS targets. We may need to defocus for the brighter targets.

What is the required slit width? (Motohara-san)
—> 10-12 arcsec in our previous MOIRCS observation. 

#15:20 "Time-Domain Science with Subaru/SWIMS", Yuu Niino (U. of Tokyo)

#15:40 "Swimming through the interstellar medium in galaxies”, Toshiki Saitoh (MPIA)
0.2 arcsec is too high for SWIMS. (Tadaki-san)
Good science case for GLAO!

What is the redshift range? Do you have the targets matched with NB filters on SWIMS?  (Motohara-san) 
—> Should be fine.  

Velocity resolution is different between NIR spectroscopy and ALMA. Isn’t it a problem for your science? (Izumi-san)
—> I will focus on the spatial distribution of ionized gas, i.e., NB imaging observation.

H-alpha emission from MUSE is useless? (Tanaka-san)
—> MUSE+AO is limited to bright targets. Pa-alpha observation is required for our ULIRG project. 

#16:00 "SWIMS views of low-luminosity quasars at z>6", Masafusa Onoue (MPIA)
Spectral resolution of SWIMS is enough (R~1000)? High spectral resolution would be important. (Tanaka-san)
—> For science about the absolution lines, higher spectral resolution (X-shooter or MOSFIRE; R~3000-5000) is required. 

Do you have any plan to install higher spectral resolution grism? (Tanaka-san, to SWIMS team)
—> We need budget… (we have tried) (Motohara-san)

Why do you need to increase your sample size by a factor of two? (Tadaki-san)
—> We see the variety of the physical properties in our current high-z QSO sample. We want to investigate the fraction of high-z QSOs with particular physical properties with a larger sample of high-z QSOs.  

#16:30 Q&A and discussion
(Iye-san’s questions)
- Is the thickness of NB filters is correct?  
  —> Yes, we have checked the thickness, surface figure, and surface roughness. There is no problem. 

- What is the small shaded region in the left-hand-side detector?
 —>  Unstable baseline level of detector 
         This region is masked in the pipeline. 

- Can exposure time of blue and red be controlled independently? 
  —> Yes. 
         e.g., a single longer exposure in blue-arm and multiple shorter exposures in red-arm 

Wavelength gap of the two detectors. How can we avoid this in spectroscopic observations? 
—> Shift x-axis direction when observing. But it takes x2 observing time.(?)
      When you observe a single object, the crowded OH sky line regions can be shifted to the gap.  

(Motohara-san comments)
Construction of TAO is now suspended due to the COVID-19 situation. ~ 6 months? 

SWIMS-MOIRCS comparison
Throughput comparison in spectroscopic obs? Especially J-band?
—> Sensitivity is comparable. 
       Maybe similar between SWIMS and MOIRCS but please check the website. 
- IFU timeline? 
Huge uncertainty but from 2023 hopefully… 

- High resolution grism? LS GRISM (R=3000)
  We should consider grant application for new grism
—>  We cannot install new grism during SWIMS is mounted on Subaru. (Motohara-san)

VPH grism is better than LS grism for Swims. But VPH grism has absorption in K band.

- How to form/join science teams (PI instrument policy)? 
  Please contact Motohara-san when you applying to SWIMS. 

- Next science workshop? 
  in 2021? 

- Buy more detectors? 
  AUS-LIEF proposal. If it is successful, we can double the FoV. 
 —> We will also apply for KAKENHI or other grants. 

- Open-use policy of SWIMS on TAO?
—> Please think about using TAO beyond Subaru. 
      33% open-use time for Japanese community. 
      + Another 42% TAO project time, large legacy survey.  

Science operation of SWIMS and PFS is overlapped. Wavelength coverage is complementary. Is it possible to manage synergetic observation with PFS and SWIMS? 
—> FoV is totally different. Arrangement of observations is difficult…?
—> Follow-up with SWIMS of interesting sources found by PFS is interesting. 

Current schedule of PFS first light? 
—> science operation from 2023 (Moritani-san)
—> matched with SWIMS operation on TAO. Good synergy. 
—> Who should I contact? 
—> Tamura-san 

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Last-modified: 2020-07-27 (月) 19:03:52