. . Prop. #:

Panel: G

Semester 2015A CHILEAN NATIONAL TAC

Deadline: October 12, 2014, 20:00

Submit your proposal at http : //www.das.uchile.cl/cntac/form prop cntac.php

1. Title

Washington Photometry For High Fidelity APOGEE-2 Targeting of Magellanic Cloud Giants

2. Abstract

The second phase of the Apache Point Observatory Galactic Evolution Experiment of the Sloan Digital SkySurvey - IV (SDSS-IV/APOGEE-2) will include a southern component that will observe ∼5,000 RGB starsin the Magellanic Clouds (MCs). This will be the first high-resolution (R=22,500) and high-S/N (S/N≥100)survey with precise stellar parameters and elemental abundances of the MCs. APOGEE-2S will spend ∼200hours in ∼30× 2◦-diameter fields mapping the chemical patterns of the MCs to large radii, allowing us tomeasure detailed abundances for many important elements over a wide galactocentric region. A sample ofclusters covering a range of ages will also be targeted to explore the chemical evolution of both Clouds. Tominimize contamination due to foreground dwarfs, especially for metal-poor MC stars, we propose to carry outWashington M , T2 and DDO51 photometry, which is the most efficient technique to separate these stars.This will allow us to make optimum use of APOGEE-2S time. We were awarded the highest grade for thisproject last semester and initially all 9 nights requested, but due to poor CNTAC administration ended upwith only 6 nights. We here request the additional 3 nights needed to complete the project.

3a.Number of requested nights, or hours, on each telescope/radiotelescope (see also #15)

CTIO

Blanco SOAR 1.5m 1.3m 0.9m LCO-GTN PROMPT

Curtis-Schmidt SARA

LCO

Baade Clay du Pont Swope Warsaw

National Telescopes

Armazones Danish EULER REM TAROT ESO-

Schmidt

Curtis-Schmidt

TRA-PPIST

MPG2.2m

3n

mini-TAO

Radio

ASTE NAN-TEN2

3b.Instrument(s) requested

WFI

4. Principal investigator

Name Douglas Geisler

e-maila dgeisler@astroudec.cl

Phone 56-41-2203092

Institute Universidad de Concepcion

Address Departamento de Astronomıa

aInstitutional e-mail required

^

Status (A,S,V): A 5. Co-investigators (names and institutions)

David L. Nidever (University of Michigan)Ricardo R. Munoz (Universidad de Chile, Santiago)Steven R. Majewski (University of Virginia)Roger Cohen (Univ. Concepcion, Chile)^Cesar Munoz (Univ. Concepcion, Chile)^Francesco Mauro (Univ. Concepcion, Chile)Sandro Villanova (Univ. Concepcion, Chile)Heinz Frelijj (Univ. Concepcion, Chile)^Juan Claria (Observatorio Astronomico de Cordoba)Celeste Parisi (Observatorio Astronomico de Cordoba)Tali Palma (Observatorio Astronomico de Cordoba)Andrea Ahumada (Observatorio Astronomico de Cordoba)

1

6a. Preferred months

first choice: Sep second choice:

6b. Other scheduling constraints (use also box 16)

We need to observe the SMC this run.

7. Moonlight constraints

No restriction

Max. # of days from new moon 10

Dark time is preferred, but gray time would be accept-able.

8a. Past and future of this project

i) Time already awarded to this project: 6

ii) Time required to complete this project(excluding this semester): None

8b. Long-term status request∗

∗Refer to the CNTAC policy for long-term programs.

9. Service/remote observing

Mark if this is a service/remote observing proposal

10a. If this proposal is part of a MSc or PhD thesis project in a Chilean institution, write here the name of thestudent, the thesis title, and briefly describe the importance of the requested observations to achieve thegoals of the thesis.

Cesar Munoz is a PhD student and Heinz Frelijj is a beginning Master’s student who are both working withus on star clusters. The proposed observations could well become part of one or both of their theses. Weanticipate that one or more additional undergraduate and/or graduate students will become involved in thisproject as well.

10b. Describe how the proposed observations complement data from non-CNTAC facilities. For each of thelatter, indicate the nature of the observations (yours or those of others), and describe the importance of theobservations proposed here in the context of the entire program.

The SDSS-IV/APOGEE-2S survey to be carried out with the DuPont telescope at Las Campanas will include∼200 hours to obtain high-S/N , high-resolution observations of ∼5,000 red giant branch stars in the MC thatwill be used to derive accurate RVs (to ∼0.1 km/s) and precise abundances of 15 elements. The WashingtonM, T2 and DDO51 photometry that we request in this proposal is required to weed out contaminatingforeground Milky Way dwarfs and obtain a high fidelity sample of MC giants.

2

11a. CNTAC observing time allocated **to this particular project** in the last 2 years

Proposal code Proposal title

CN2014B-66 Washington Photometry For High Fidelity APOGEE-2 Targeting of Magellanic Cloud Giants

Dates Telescope Awarded time Loss (%) Reason(s)

Dec. 27, 2014 - Jan. 1,2015

MPG2.2m 6n Future observations

11b. Brief description of the status of this project, including publications.

The PI received the following message on Aug. 15, 2014:

CNTAC proposal CN2014B-66Dear Doug,The Chilean Telescope Allocation Committee (CNTAC) has reviewed your proposal titled ”WashingtonPhotometry For High Fidelity APOGEE-2 Targeting of Magellanic Cloud Giants” submitted to considerationfor semester 2014B. I am pleased to inform you that 9 nights were allocated to your program. Whenthe program is available I will let you know.... Your grade was 1.0 on a scale from 1 (outstanding) to 5(unfeasible) with an average of 2.5. The subscription factor on the 2.2m telescope was 3.50; your proposalwas ranked 1 out of 19 proposals received for that telescope.Sincerely,Diego MardonesOn Behalf of the CNTAC(NB - boldface added)

The PI asked for clarification of the vague content of this letter regarding scheduling. After waiting foranother week or so without further response, the PI contacted Roland Gredel, who is in charge of theMPG2.2m schedule, who sent this email Aug. 26:

Hi Doug,unfortunately I did not get feedback from the CNTAC until early August, so right now the scheduling ofChilean programmes might not be ideal. I am waiting for a response from CNTAC... The CNTAC processhas been sub-optimal this time and I am going to raise this issue with Chilean collegues in November whenI am in Santiago.All the best,Roland

On Sept, 3, the PI received this message from the CNTAC:

Estimado Doug,Ahora termino las noticias, buenas y no tanto. Tienes asignadas las noches de Dec 27, 28, 29, 30, 31, 2014y Jan 1, 2015... Las buenas noticias son el tiempo asignado. Las malas son que solo pude darte 6 nochesdebido a las condiciones de Luna y el calendario disponible, y que incluye lamentablemente la noche de anyonuevo.Saludos,Diego

The PI and colleagues were understandably upset at this decrease in their time assignment, as wellas the fact that they had requested their first choice observing period as November in order to beable to observe both MCs and were given late December, meaning that the SMC would only be ob-servable for a very short time. All of this despite having received the highest grade on the telescope, aperfect 1.0! The PI subsequently checked again with Roland Gredel, who sent this message the following day:

Hi Doug,yes, since I had not received any input from the CNTAC before August, I had to block-schedule Chileantime. I had communicated this to the chair of the CNTAC but he has not responded yet. I am really sorrythose issues cause uncertainty. As mentioned before, I am going to express my concerns about the presentprocess verbally, in November, when in Chile.All the best,Roland

The net result is that the highest ranked proposal on the MPG2.2m, which was initially assigned the fullrequest of 9n, received a final allotment of only 6n at a scientifically (and personally) unfavorable time, dueto tardiness by the CNTAC administration in carrying out their obligations. We feel this is an unacceptablesituation and therefore are submitting this proposal to recover the lost nights and the ability to observe theSMC. Note that the assigned nights are still in the future.

3

11c. Other publications in the course of the past 3 years on the topic of this proposal (including article titles).

Parisi, M. C., Geisler, D., Carraro, G. et al. 2014, AJ, 147, 71: Age Determination of 15 Old to Intermediate-ageSmall Magellanic Cloud Star Clusters

Cummings, Jeffrey D.; Geisler, D.; Villanova, S.; et al. 2014, AJ, 148, 27: Uncovering Multiple Populationswith Washington Photometry. I. The Globular Cluster NGC 1851

Bovy, Jo; Nidever, David L.; Rix, Hans-Walter; et al. 2014, ApJ, 790, 127: The APOGEE Red-clump Catalog:Precise Distances, Velocities, and High-resolution Elemental Abundances over a Large Area of the Milky Way’sDisk

Anders, F., Chiappini, C., Santiago, B. X. et al. 2014, A&A, 564, 784: Chemodynamics of the Milky Way. I.The first year of APOGEE data

Hayden, M. R., Holtzman, J. A., Bovy, J. et al. 2014, AJ, 147, 115: Chemical Cartography with APOGEE:Large-scale Mean Metallicity Maps of the Milky Way Disk

Ahn, C. P., Alexandroff, R., Allende Prieto, C. et al. 2014, ApJS, 211, 17: The Tenth Data Release of the SloanDigital Sky Survey: First Spectroscopic Data from the SDSS-III Apache Point Observatory Galactic EvolutionExperiment

Epstein, C. R., Elsworth, Y. P., Johnson, J. A. et al. 2014, ApJ, 785, 28: Testing the Asteroseismic Mass ScaleUsing Metal-poor Stars Characterized with APOGEE and Kepler

Eikenberry, S. S., Chojnowski, S. D., Wisniewski, J. et al. 2014, ApJ, 784, 30: Discovery of Two Rare RigidlyRotating Magnetosphere Stars in the APOGEE Survey

Nidever, D. L., Monachesi, A., Bell, E. F. et al. 2013, ApJ, 779, 145: A Tidally Stripped Stellar Component ofthe Magellanic Bridge

Desphande, R., Blake, C. H., Bender, C. F. et al. 2013, AJ, 146, 156: The SDSS-III APOGEE Radial VelocitySurvey of M Dwarfs. I. Description of the Survey and Science Goals

Majewski, S. R., Hasselquist, S., Lokas, E. L. et al. 2013, ApJ, 777, 13: Discovery of a Dynamical Cold Pointin the Heart of the Sagittarius dSph Galaxy with Observations from the APOGEE Project

Frinchaboy, P. M., Thompson, B., Jackson, K. M. et al. 2013, ApJ, 777, 1: The Open Cluster ChemicalAnalysis and Mapping Survey: Local Galactic Metallicity Gradient with APOGEE Using SDSS DR10

Palma, T., Claria, J. J., Geisler, D. et al. 2013, A&A, 555, 131: A sample of relatively unstudied star clustersin the Large Magellanic Cloud: fundamental parameters determined from Washington photometry

Meszaros, Sz., Holzman, J., Garcıa Perez, A. E. et al. 2013, AJ, 146, 133: Calibrations of AtmosphericParameters Obtained from the First Year of SDSS-III APOGEE Observations

Zasowski, G., Johnson, J. A., Frinchaboy, P. M. et al. 2013, AJ, 146, 81: Target Selection for the ApachePoint Observatory Galactic Evolution Experiment (APOGEE)

Piatti, A. E. & Geisler, D. 2013, AJ, 145, 17: The Age-Metallicity Relationship of the Large Magellanic CloudField Star Population from Wide-field Washington Photometry

Garcıa Perez, A. E., Cunha, K., Shetrone, M. et al. 2013, ApJ, 767, 9: Very Metal-poor Stars in the OuterGalactic Bulge Found by the APOGEE Survey

Ahn, C. P., Alexandroff, R., Allende Prieto, C. et al. 2013, ApJS, 203, 21: The Ninth Data Release of theSloan Digital Sky Survey: First Spectroscopic Data from the SDSS-III Baryon Oscillation Spectroscopic Survey

Bovy, J., Allende Prieto, C., Beers, T. C. et al. 2012, ApJ, 759, 131: The Milky Way’s Circular-velocity Curvebetween 4 and 14 kpc from APOGEE data

Wilson, J., Hearty, F., Skrutskie, M. F. et al. 2012, SPIE, 8446, 0H: Performance of the Apache Point Obser-vatory Galactic Evolution Experiment (APOGEE) high-resolution near-infrared multi-object fiber spectrograph

Nidever, D. L, Zasowski, G., Majewski, S. R. et al. 2012, ApJ, 755, 25: The Apache Point Observatory GalacticEvolution Experiment: First Detection of High-velocity Milky Way Bar Stars

Mateluna, R., Geisler, D., Villanova, S. et al. 2012, A&A, 548, 82: Chemical abundances in the old LMCglobular cluster Hodge 11

Nidever, D. L., Majewski, S. R., Munoz, R. R. et al. 2011, ApJ, 733, 10: Discovery of a Large Stellar PeripheryAround the Small Magellanic Cloud

Piatti, A. E., Geisler, D., & Mateluna, R. 2012, AJ, 144, 100: A Washington Photometric Survey of the LargeMagellanic Cloud Field Star Population

Piatti, A.E., Bica, E., Claria, J.J., et al. 2011, MNRAS, 417, 1559: Washington photometry of 14 intermediate-age to old star clusters in the Small Magellanic Cloud

4

12. Description of the programme (1 page of text and up to 2 pages for references, tables and figures.)

A) Scientific rationaleThe Magellanic Clouds (MCs) are a unique local laboratory for studying the formation and chemodynamicalevolution of dwarf galaxies in exquisite detail. As the closest example of an interacting pair of galaxies, theyprovide special insight into the impact of such interactions on the stellar structure and star formation histories ofgalaxies. Dwarf galaxies are also the most numerous in the Universe. However, the field of dwarf galaxy chemicalabundances is still in its infancy because the brightest stars of even the nearest dwarf galaxies are very faint. Inthe last decade, the measurement of detailed abundances of stars in Milky Way (MW) dwarf spheroidal (dSph)galaxies has begun (e.g., Shetrone et al. 2001; Geisler et al. 2005; Tafelmeyer et al. 2010). However, in generalonly a relatively small number of stars per galaxy have been measured, limiting the analysis to global properties,although sample sizes are increasing (e.g. Lemasle et al. 2012). Furthermore, the MW dSphs are low-mass (107

M�) and low star formation rate galaxies with most having little star formation in the recent past. This leavesunexplored a large range in mass — 108–1011 M� — and star formation rate - which is nicely filled by the MCs.While some abundance work has already been done on the MCs, these have been limited to only a few spatialregions or a handful of star clusters (e.g., Mucciarelli et al. 2008; Van der Swaelman et al. 2013).The SDSS-III Apache Point Observatory Galactic Evolution Experiment (APOGEE; Majewski et al. 2014) istaking NIR H-band high-S/N and high-resolution spectra of 100,000 red giant branch stars in the Milky Wayto study its kinematical and chemical structure. The full-hemisphere SDSS-IV/APOGEE-2 survey (starting mid2014) will include a southern portion (APOGEE-2S on the Las Campanas Observatory du Pont-2.5m starting2016) that will cover the MCs and obtain spectra of ∼5,000 giants extending out to the edge of the MC mainbodies. This survey will obtain spatially-resolved, detailed multi-element abundances in tens of fields (withhundreds of stars per field) covering the full spatial extent of the star forming MCs. This dataset will allowus to derive spatial abundance gradients (in radius and azimuth) that have so far not been well constrainedobservationally for dwarf galaxies. Simulations predict that radial abundance gradients should depend on mass(steeper for low-mass and flatter for high-mass) and possibly age (Bekki & Shioya 1999). The combination ofabundance gradients for the MW (∼1012 M�; from APOGEE-1+2), the LMC (∼2×1010 M�), and the SMC(∼2×109 M�) will allow us to observationally test the mass-dependence of abundance gradients for the first time.We will (1) measure detailed chemical abundance patterns in many spatial regions throughout the MCs; (2)measure the mass dependence of chemical abundance gradients using the MW and MCs; (3) derive abundancesfor one to several giants in each of a number of star clusters with a range of ages to study the chemical evolutionof the Clouds; and (4) investigate kinematics of the MCs in great detail.B) Scientific aimThe APOGEE-2S spectroscopic survey of the MCs will produce a groundbreaking dataset for the study of thesetwo nearest dwarf galaxies. But to best accomplish this requires an efficient method to separate the contaminatingforeground MW dwarfs from the MC giants that APOGEE is designed to target. The most efficient way to achievethis is using a photometric method. Geisler (1990) added the DDO 51 filter to the Washington photometricsystem specifically for the purpose of late-type dwarf - giant discrimination. The combination of WashingtonM, T2 and DDO51 photometry has been shown to be very effective at such separation (Majewski et al. 2000)(see Figure 1). This is especially important in the periphery of the MCs where the MC stellar density is low andfor metal-poor ([Fe/H]∼−2) MC stars that are rare even near the center of the MCs. The technique is mosteffective at separating solar metallicity dwarfs from low metallicity giants. Our requested photometry will providea high-fidelity catalog of MC red giant branch stars in the 30 fields that APOGEE-2S will target (see Figure 2).Fiber placement constraints will limit the number of giants we can observe within clusters to only one or a few.However, combining the detailed abundances we will measure with known ages of these clusters will allow us toinvestigate the age-metallicity distribution and chemical evolution of both Clouds in much greater detail thancurrently possible. We estimate that a large number of clusters with a range of ages will be present in our fields.Our team has extensive experience using this filter set to separate dwarfs from giants (e.g., Geisler 1990,Palma et al. 2003, Westfall et al. 2006, Munoz et al. 2006a, Majewski et al. 2009, Nidever et al. 2011) andhave found it to produce ∼95% pure giant samples. After the decommissioning of the CTIO-4m+MOSAICinstrument, the ESO-2.2m+WFI is now the best southern instrument for obtaining wide-field Washington M,T2 and DDO51 photometry for this project. We will reduce the multi-chip imaging data with the standardIRAF mscred package to produce flattened images (i.e., overscan, zero, domeflat, illum flat, etc.). We willthen use the automated DAOPHOT-based PHOTRED photometry package (described in Nidever et al. 2011)to obtain accurate WCS information for our images and produce accurate PSF photometry. An example ofPHOTRED-reduced photometry (using CTIO-4m+MOSAIC data) is shown in Figure 1. Photometry accurateto ∼2% is required for good dwarf/giant separation. We will use our nightly observations of several standard starfields (Geisler 1990) to derive photometric transformation equations with color, airmass and nightly zeropointterms. Neighboring pointings in each field will have overlap to facilitate the global photometric calibration of thedataset. The characteristic “swoosh” of the dwarf sequence in the (M − T2,M-DDO51) diagram (see bottompanel of Figure 1) will be used to correct for small photometric offsets in each pointing. Finally, we will defineregions in the CMD and color-color diagram to select giants.As explained in detail in Section 11b, this project was awarded the highest grade on this telescope last semester,a perfect 1.0, and was initially assigned all 9 nights requested but, due to poor CNTAC administration, endedup with only 6 nights at a scientifically non-optimal time. This proposal is to recover the lost nights and theability to observe the SMC.

5

Bekki, K., & Shioya, Y. 1999, ApJ, 513, 108

Geisler, D. 1990, PASP, 102, 344

Geisler, D., Smith, V, Wallerstein, G., et al. 2005, AJ, 129, 1428

Lemasle, B., Hill, V., Tolstoy, E. et al. 2012, A&A, 538, 100

Majewski, S. R. et al. 2000, AJ, 120, 2550

Majewski, S. R., Nidever, D. L. et al. 2009, IAUS, 256, 51

Majewski, S. R. et al. 2014, in preparation

Munoz, R. R., Majewski, S. R., et al. 2006, ApJ, 649, 201

Mucciarelli, A. et al. 2008, AJ, 136, 375

Nidever, D. L. et al. 2011, ApJL, 733, 10

Palma, C., Majewski, S. R. et al. 2003, AJ, 125, 1352

Shetrone, M. et al. 2001, ApJ, 548, 592

Tafelmeyer, M. et al. 2010, A&A, 524, 58

Van der Swaelman, M. et al. 2013, A&A, 560, 44

Westfall, K., Majewski, S. R., et al. 2006, AJ, 131, 375

Figure 1: Top: A Washington photometry color-magnitude diagram of the SMC. The isochrone representsthe SMC halo stellar population. Bottom: The (M-T2) vs. (M-DDO51) color-color plane in which thegiant-star locus separates from the dwarf-star locus for late-type stars. In both panels, red large dots

represent giant stars selected in the color-color plane. They clearly follow the SMCs isochrone andefficiently remove most MW-foreground contaminants in the CMD.

23

22

21

20

19

18

17

16

M

R=4.3o

[Fe/H]=−1.306 Gyr63 kpc

0 1 2(M−T2)o

−0.4

−0.2

0.0

0.2

(M−

DD

O51) o

M<20.0

Dwarfs

Giants

5a

References

Figure 2: The APOGEE-2S plan for the 30× 2◦-diameter Magellanic Clouds fields: 21 fields for the LMCwill extend out to R=10.6◦ on the major axis and R=7.4◦ on the minor axis; 9 fields will survey the SMC

out to R=4.2◦. The density of 2MASS-selected RGB stars is in grayscale and HI is shown in black contours.

−80

−70

−60

0h

2h

4h

6h

8h

21 LMC fields

9 SMC fields

Strawman 6 (30 fields)Strawman 6 (30 fields)

5b

13. List of targets (absence of a proper object list and information will weaken your proposal). You can includean hyperlink to online catalogs (e.g., Simbad, Vizier, NED, etc.)

Name α δ Epoch Mag. Additional Information (e.g., redshift, red-dening, angular size, etc.)

SMC1 00 40 41.40 -69 46 35.45 J2000 18.0SMC2 00 52 43.99 -72 49 41.99 J2000 18.0SMC3 01 09 43.93 -75 49 01.43 J2000 18.0SMC4 01 14 31.41 -68 40 14.50 J2000 18.0SMC5 01 31 07.08 -71 32 38.28 J2000 18.0SMC6 01 53 27.64 -74 17 41.22 J2000 18.0SMC7 00 03 51.80 -70 25 43.94 J2000 18.0SMC8 00 09 38.84 -73 35 51.91 J2000 18.0SMC9 00 18 04.06 -76 45 08.03 J2000 18.0

14. Observational strategy and justification of instrument and requested time (including overheads).

Time Justification: The exposure time required for a single pointing is determined by the necessity to obtainhigh signal-to-noise photometry to the faint end of the SMC red giant branch stars that APOGEE-2 willtarget. With APOGEE-2S we will target MC red giant branch stars down to H∼14.2 and possible fainter.To be safe we will want to have good dwarf/giant separation well below that magnitude, down to H=15.0.For red giants this corresponds to M=18.0. At least ∼2% photometric precision is required in DDO51 and1% precision in M and T2 at the faint end for efficient dwarf/giant separation in the (M-T2) vs. (M-DDO51)color-color plane (see Figure 1 lower panel). From our previous experience with similar observations, thismeans obtaining S/N=50 photometry with the intermediate-band DDO51, and S/N=100 photometry withthe far less time-consuming broad-band M and T2 (same as Ic) filters so as to curb the uncertainties on theM-DDO51 color of stars, essential for this analysis. Using the WFI exposure time calculator and assuminggrey time (7 days from new moon), a reasonable 1.2” seeing for La Silla and an airmass of 1.7 for thesouthern declinations of our targets, this leads to exposure times of 27s, 29s, and 62s for M , T2 and DDO51respectively. Shrinking the DDO51 exposure time would be very detrimental to the program as we would nothave an efficient giant/dwarf discrimination, severely impacting our ability to create a high-fidelity MC giantstarget list for APOGEE-2S. Accounting for the overhead (1 min for telescope slewing, 1 min for guide-staracquisition, 2 min for filter changes, and 2 min readout time) leads to 8 minutes of telescope time perpointing. The 2◦-diameter APOGEE-2S field size can be covered with 14 WFI pointings with considerableoverlap. Therefore, it will take 112 min to cover one APOGEE-2S field with WFI. For the 9 SMC fields shownin Figure 2 this adds up to about 18 hours. We will also require 5–6 standard star field observations for eachnight which will require an additional ∼1 hour per night. We can also observe additional LMC fields at theend of the night. We request 3 nights total to also ensure against weather problems in order to completethis project.Lunar Phase Justification: Our use of both reasonably shallow broad-band optical photometry (WashingtonM and T2 filters) and the intermediate-band DDO51 filter means that we do not need dark time for thisproject. The necessity of having as good photometry as possible to discriminate dwarf stars from giant stars(see Figure 1), however, means that we need grey time for this program.

6

15a. Optical/IR telescopes: requested instrument(s) setup

Direct photometry Washington M , T2 (Ic), and DDO51 (513) filters.

15b. Radio

Telescope LST interval Obs. periods Total # of hours Type Lines Rec/Spec (bandwidth)

ASTE

NANTEN

POLARBEAR

ACT N/A

16. Scheduling constraints, special requirements and other remarks

We need to observe the SMC (RA≈0h). The 6 nights allotted the previous semester are in late December -early January and we will not be able to observe the SMC during most of these nights.

17. Backup program (if proposal needs outstanding weather)

7

CNTAC LATEX style file vCNTAC 2015A September 2014.