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instruments [2022/03/11 00:29] – holtzinstruments [2026/01/30 05:52] (current) – external edit 127.0.0.1
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 ===== Instrument upgrades / New instruments ===== ===== Instrument upgrades / New instruments =====
  
-==  Fiber feed from 3.5m to SDSS/APOGEE ==+====  Fiber feed from 3.5m to SDSS/APOGEE ====
  
-== White Paper: NETWORKED ASTRONOMY AT APACHE POINT OBSERVATORY ==+=== White Paper: NETWORKED ASTRONOMY AT APACHE POINT OBSERVATORY ===
  
 **ABSTRACT** **ABSTRACT**
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 plane of the NMSU 1 m telescope where they will replace and improve the existing fiber run. plane of the NMSU 1 m telescope where they will replace and improve the existing fiber run.
  
-The full paper can be downloaded here. +The full paper can be downloaded {{:wiki:inst:apofiber.2.pdf|here}}
- +
-http://astronomy.nmsu.edu:8000/apo-wiki/attachment/wiki/Instruments/APOfiber.2.pdf +
- +
- +
-**Assumed Parameters for APOGEE:**+
  
 +== Assumed Parameters for APOGEE ==
   * R=22,500 from 1.51 - 1.70 um,  300 2" dia fibers in SDSS 2.5m f/5 focal plane   * R=22,500 from 1.51 - 1.70 um,  300 2" dia fibers in SDSS 2.5m f/5 focal plane
- 
   * ~15% throughput --> S/N = 100/pix for H > 12.2 in t = 3 hrs   * ~15% throughput --> S/N = 100/pix for H > 12.2 in t = 3 hrs
- 
   * radial velocity to 100 m/sec   * radial velocity to 100 m/sec
  
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   * Single fiber: 0.7" at F/10, 1.4" at f/5 (i.e., with focal reduction)   * Single fiber: 0.7" at F/10, 1.4" at f/5 (i.e., with focal reduction)
- 
   * IFU 1.4" spaxels, 217 elements, ~39" across, lenslet array in front for ~100% fill factor and f/5 conversion   * IFU 1.4" spaxels, 217 elements, ~39" across, lenslet array in front for ~100% fill factor and f/5 conversion
- 
   * MOS ~ 200-300 1.4" fibers (with lenslets) in 8' FOV (pretty tightly packed!) or ~30 Randomly targeted objects (e.g in 7-fiber bundles) in 8' FOV.   * MOS ~ 200-300 1.4" fibers (with lenslets) in 8' FOV (pretty tightly packed!) or ~30 Randomly targeted objects (e.g in 7-fiber bundles) in 8' FOV.
  
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 John Bally, Kevin Bundy, Jon Holtzman, Don York, Jennifer Sobeck John Bally, Kevin Bundy, Jon Holtzman, Don York, Jennifer Sobeck
  
-**APOGEE Dense Pack IFU**+== APOGEE Dense Pack IFU ==
  
   * Nearby Galactic Star and star clusters [Bally ~ See attached]   * Nearby Galactic Star and star clusters [Bally ~ See attached]
- 
   * Nearby HII regions and post-main-sequence objects [Bally ~ See attached]   * Nearby HII regions and post-main-sequence objects [Bally ~ See attached]
- 
   * Young Massive Clusters (YMCs) and Super Star Clusters (SSCs) [Bally ~ see attached]   * Young Massive Clusters (YMCs) and Super Star Clusters (SSCs) [Bally ~ see attached]
- 
   * Massive Stellar Transient Nearby Galaxies [Bally ~ See attached]   * Massive Stellar Transient Nearby Galaxies [Bally ~ See attached]
- 
   * Individual abundances in globular cluster stars from near-IR, perhaps from an IFU [Holtzman]   * Individual abundances in globular cluster stars from near-IR, perhaps from an IFU [Holtzman]
- 
   * Integrated light of globular clusters   * Integrated light of globular clusters
- 
   * Dwarf spheroidals [Holtzman, Sobeck]   * Dwarf spheroidals [Holtzman, Sobeck]
- +  * Dwarf galaxies [Bundy, Holtzman]
-  *  Dwarf galaxies [Bundy, Holtzman] +
   * Extragalactic (Emission lines, Stellar populations, and Stellar Dynamics) [Bundy ~ See below]   * Extragalactic (Emission lines, Stellar populations, and Stellar Dynamics) [Bundy ~ See below]
  
- **Single object science** +== Single object science ==
  
   * Abundances of Hipparcos sub-giants [Holtzman]   * Abundances of Hipparcos sub-giants [Holtzman]
- 
   * Radial velocity monitoring of late-type stars    * Radial velocity monitoring of late-type stars 
- 
   * supernova followup in H band   * supernova followup in H band
- 
   * Survey of B[e] stars [Chojnowski]   * Survey of B[e] stars [Chojnowski]
  
-**APOGEE MOS** +== APOGEE MOS ==
  
   * The nature of star and clusters in the Central Molecular Zone (CMZ) and nearby starburst galaxies [Bally ~ See attached]   * The nature of star and clusters in the Central Molecular Zone (CMZ) and nearby starburst galaxies [Bally ~ See attached]
- 
   * Blind Emission-Line Searches of Deep Extra-Galactic Fields [Bally ~ See attached]   * Blind Emission-Line Searches of Deep Extra-Galactic Fields [Bally ~ See attached]
  
-**Future Fiber Feeds**+== Future Fiber Feeds ==
  
   * A Visual-Wave fiber bundle for the APO 3.5 meter [Bally ~ See attached]   * A Visual-Wave fiber bundle for the APO 3.5 meter [Bally ~ See attached]
- 
   * Visual wave band IFU observations of nebula [York ~ See below]   * Visual wave band IFU observations of nebula [York ~ See below]
  
-=== Detailed Science Cases ===+== Detailed Science Cases ==
  
 A number of science cases have been put forward by John Bally in an attached document ''"Science Case for a~300 fiber connection from the APO 3.5m to the SDSS spectrograph"'' for details please see the attachments of this page. A number of science cases have been put forward by John Bally in an attached document ''"Science Case for a~300 fiber connection from the APO 3.5m to the SDSS spectrograph"'' for details please see the attachments of this page.
  
- +== Single object possibilities ==
- +
-==== Single object possibilities ====+
  
 A single-object 3.5m feed is desirable for objects that are sufficiently spaced in the sky such that observing with the 2.5m does not offer benefits from wide field and for specific single objects of interest. The 3.5m would also potentially allow observations of fainter objects than can be done with the 2.5m. Note that the throughput gain comes from telescope area (3.5/2.5)^2^ = 1.96  (0.73 mag fainter) and also from the fact that the corrector at the 2.5m is estimated to absorb ~30% of the light in the H band (another 0.3 mag). On the other hand, there might be some additional light losses from a longer fiber run, especially if it were to involve multiple connectors. Also to avoid seeing losses that would be larger with the 1.4" fibers even at F/5 from the 3.5m, one would want to consider a lenslet array in from of a fiber bundle, such that light was collected over multiple fibers without any loss between fibers. This might lead to additional throughput gains. But ballpark, a 3.5m feed would allow observations 1 mag fainter than at the 2.5m in the same time, e.g. S/N=100/pixel at H=13.2 in 3 hours, or S/N=100/pixel at H=11 in 1 hour.  A single-object 3.5m feed is desirable for objects that are sufficiently spaced in the sky such that observing with the 2.5m does not offer benefits from wide field and for specific single objects of interest. The 3.5m would also potentially allow observations of fainter objects than can be done with the 2.5m. Note that the throughput gain comes from telescope area (3.5/2.5)^2^ = 1.96  (0.73 mag fainter) and also from the fact that the corrector at the 2.5m is estimated to absorb ~30% of the light in the H band (another 0.3 mag). On the other hand, there might be some additional light losses from a longer fiber run, especially if it were to involve multiple connectors. Also to avoid seeing losses that would be larger with the 1.4" fibers even at F/5 from the 3.5m, one would want to consider a lenslet array in from of a fiber bundle, such that light was collected over multiple fibers without any loss between fibers. This might lead to additional throughput gains. But ballpark, a 3.5m feed would allow observations 1 mag fainter than at the 2.5m in the same time, e.g. S/N=100/pixel at H=13.2 in 3 hours, or S/N=100/pixel at H=11 in 1 hour. 
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 Another application might be a survey of B[e] stars, which are B-type emission line stars that differ from classical Be stars due to the presence of forbidden emission lines and strong IR excesses. These features are attributed to a circumstellar dust component not present in the case of classical Be stars. The ~100 or so known B[e] stars are a heterogeneous group often found to be supergiants (sgB[e]), pre-main sequence (HAeB[e]), or compact planetary nebulae (cPNB[e]). However, the fact that ~50% of them remain unclassified (unclB[e]) is a testament to the complexity and richness of the emission line spectra, and also to the difficulty of conducting a uniform survey given the isolated nature of the stars. On average, B[e] stars are almost 4 magnitudes brighter in the H-band than in V-band, making them ideal targets for NIR spectroscopy. For more information, see [http://adsabs.harvard.edu/abs/1998A%26A...340..117L Lamers et al. 1998], and Miroshnichenko et al. 2007 [http://adsabs.harvard.edu/abs/2007ApJ...667..497M A] + [http://adsabs.harvard.edu/abs/2007ApJ...671..828M B]. Another application might be a survey of B[e] stars, which are B-type emission line stars that differ from classical Be stars due to the presence of forbidden emission lines and strong IR excesses. These features are attributed to a circumstellar dust component not present in the case of classical Be stars. The ~100 or so known B[e] stars are a heterogeneous group often found to be supergiants (sgB[e]), pre-main sequence (HAeB[e]), or compact planetary nebulae (cPNB[e]). However, the fact that ~50% of them remain unclassified (unclB[e]) is a testament to the complexity and richness of the emission line spectra, and also to the difficulty of conducting a uniform survey given the isolated nature of the stars. On average, B[e] stars are almost 4 magnitudes brighter in the H-band than in V-band, making them ideal targets for NIR spectroscopy. For more information, see [http://adsabs.harvard.edu/abs/1998A%26A...340..117L Lamers et al. 1998], and Miroshnichenko et al. 2007 [http://adsabs.harvard.edu/abs/2007ApJ...667..497M A] + [http://adsabs.harvard.edu/abs/2007ApJ...671..828M B].
  
-==== Extragalactic ====+== Extragalactic ==
  
 //Prepared by Kevin Bundy// //Prepared by Kevin Bundy//
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   - Large (much larger?) fiber apertures: ?   - Large (much larger?) fiber apertures: ?
  
- +== More about APOGEE applicability for extragalactic studies ==
- +
-==== More about APOGEE applicability for extragalactic studies ====+
  
 //Prepared by Dmitry Bizyaev// //Prepared by Dmitry Bizyaev//
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 {{inst:m32_2.png}} {{inst:m32_2.png}}
- 
  
 Table: Signal-to-noise per pixel from extragalactic objects with APOGEE on 2.5m  Table: Signal-to-noise per pixel from extragalactic objects with APOGEE on 2.5m 
- 
 ||Object    |SB(H),mag/sqarcsec | SNR/pix, 1 visit (67 min)|| ||Object    |SB(H),mag/sqarcsec | SNR/pix, 1 visit (67 min)||
 ||M32 center   |11.42    |     350|| ||M32 center   |11.42    |     350||
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 ||Off-center |SB(H),mag/"**2 | SNR/pix,7 combined visits|| ||Off-center |SB(H),mag/"**2 | SNR/pix,7 combined visits||
 ||M32     |    ~18.2      |      4|| ||M32     |    ~18.2      |      4||
- 
  
 The central surface brightness in the H-band is taken from the 2MASS Atlas of Large Galaxies. The central surface brightness in the H-band is taken from the 2MASS Atlas of Large Galaxies.
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 using only a few spaxels out of 300. using only a few spaxels out of 300.
  
- +== Optical IFU for Nebula Work ==
- +
-==== Optical IFU for Nebula Work ====+
  
 //Prepared by Don York// //Prepared by Don York//
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 1/20/15 - I've updated the budget for the 'bare bones' option based on input from Mark and Bill - NKM 1/20/15 - I've updated the budget for the 'bare bones' option based on input from Mark and Bill - NKM
- 
  
 {{medialist>wiki:inst:*}} {{medialist>wiki:inst:*}}
 +
instruments.1646958575.txt.gz · Last modified: by holtz
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