Multi-Scale
Star Formation
April, 3-7th 2017
Morelia, Michoacán. México
Our understanding of the physical and chemical processes that culminate in the formation of stars and stellar clusters in the Universe has undergone great progress in recent years, both from observations and from theory and simulations. One of the main realizations is that the star-formation process involves a continuous gas flow from galactic (kpc) scales down to stellar (AU) scales. However, there is still a lack of exchange from the different communities performing research in this topic at different characteristic scales.
Given the need to cross-link processes over this wide range of scales, this conference aims at bringing together experts that work in all the relevant scales related to star formation, with the hope that researchers working in a given scale range will bring in their point of view to workers at other scales, improving our understanding of star formation as a broader theme. To achieve this, each session will contain contributed talks from different scales, although preserving an underlying scheme. The invited talks will seek to relate a specific topic to the broader context. There will also be time allocated for two or three one-hour discussion sessions to exchange ideas on the relation of a specific scale to the others.
The conference will be held at the University Cultural Center (Centro Cultural Universitario) of the "Universidad Michoacana de San Nicolás de Hidalgo" (UMSNH). This is a beautiful colonial-style building with an auditorium for 300 people and several smaller meeting rooms, located at the heart of downtown Morelia, within 2 blocks of the Cathedral, and within walking-distance from several hotels. For more information, click on the following link:
http://www.mexicoescultura.com/recinto/55277/en
The city of Morelia is the capital of the state of Michoacán in central México. Before the spanish colonization, the area was inhabited by the purépecha and the matlatzinca cultures, but no major cities were founded in the valley during this time. The spanish founded a settlement here in 1541 with the name of Valladolid. After the mexican war of independence, the city was renamed Morelia in honor of José María Morelos, one of the main leaders of the war. Morelia is currently a beautiful colonial city, with an ordinance that no building should be taller than its cathedral's towers, to preserve its majestic dominance over the landscape. Morelia was declared a UNESCO World Heritage Site in 1991.
For more information about Michoacán, please visit the site Visit Michoacan (spanish only). Or download the Travel Guide (English/Spanish).
Taxi Sharing
Dear participants, in the following google document you will be able to share a taxi or take a place of one already shared.
By plane
Morelia is served by General Francisco Mújica international airport (MLM) which is located at the edge of town. Going to the city center takes about half an hour. Book the taxi within the terminal (in “Taxi autorizado”) and take the ticket to the taxi area (~400 MXN or ~20 USD). There are daily international flights from Los Angeles, Dallas-Fort Worth, Houston, and Chicago-Midway which lead to Morelia's international airport, as do commuter flights from Guadalajara, Mexico City, Monterrey, and Tijuana.
Arriving to Mexico City airport and then by bus to Morelia
Mexico City has 4 large bus stations (one for each cardinal direction). The best one to come to Morelia is the westward one ("Terminal Poniente", also called "Observatorio"). There, the Autovias and ETN lines depart to Morelia each half an hour or so. ETN is a bit more expensive and more comfortable, but both are OK. Several buses come from the north bus station as well, but much more sparse schedule.
For more information about buses schedule you can visit the buses web site:
To take the taxi from Mexico City airport to the bus station, pay the ticket in one of the authorized booths inside the terminal. There are several booths: one in baggage claim, one just outside customs, and another one just before the exit where the taxis wait. In the booth there are several brands of taxis. Yellow Cab and Nueva Imagen usually have the most cars available at a given time.
Once in Morelia bus station, there is a taxi booth just when you come out to the main hall. Unlike in Mexico City airport, the booth person here most likely will not speak English, so a print-out of your hotel reservation address would help a lot if you don't speak Spanish.
Arriving directly to Morelia airport
There is booth for authorized taxis just outside customs. Probably the booth person and the driver will know some English, but a print-out of your Hotel reservation with address will be helpful. They may ask you if you want to go by the free or the toll highway. The toll-highway route is about 20 min faster and more comfortable. The price difference is about 3 to 5 USD.
By bus
Deluxe buses serve Morelia from all parts of the country, and Morelia's state-of-the-art bus station, located in the north-western part of the city. The bus station consists of separate terminals for first-class and second-class buses. ETN and Autovias bus companies are suggested. It is easy to reach Morelia from either Mexico City or Guadalajara. The bus trip from Guadalajara is about 3-1/2 hours. From Mexico City the trip is around 4 hours. They are services every 15-30 minutes and they leave Mexico City from bus terminal “Poniente” (also known as “Observatorio”). Single tickets cost ~500 pesos (~26 USD).
Moving around
The conference auditorium is located at the city center. Suggested hotels and restaurants are all at walking distances. Buses, “combis” (small vans) and taxis are Morelia’s main means of public transportation. Combis are a good way to see the smaller roads and backstreets of the city. Various destinations are usually indicated on the windshield of these mini-vans. A ride within the city costs ~10 MXN (~0.5 USD). Get in, grab a handle and sit down before the driver speeds up, and then give your money directly to the driver, or to someone else to pass it to the driver for you (you can ask the person “Si no le molesta, por favor”, basically: “Please, if you don’t mind”). Above your head you will find a buzzer to get out at the next corner, or you can simply ask “en la próxima esquina, por favor” (“next corner please”). Taxis are also plentiful and inexpensive (less than 100 MXN or ~5 USD), operating on zone fares. As elsewhere in Mexico, make sure to determine the price before getting into the taxi. Driving in the city is not easy, but with patience you can. Driving in and around Morelia differs little from driving in any urban area. However, there is an “uno y uno” protocol in place. Drivers are actually quite respectful and obey this “one and one” rule, where at an intersection, fall into line, with one vehicle at a time from each direction driving through the intersection. Please be aware that the “centro histórico” (downtown) area rarely has any avaiable parking spaces, but there are several parking lots in the area.
Visa
Some participants may require a visa in order to enter Mexico. Official information of the countries for which a visa is required is available in the following link (Spanish only):
http://www.inm.gob.mx/gobmx/word/index.php/paises-requieren-visa-para-mexico/
If you happen to require a visa, please contact the LOC for assistance.
We provide a map with some of the hotels in the downtown Morelia area, together with the location of the conference venue, on the conference website. Participants should contact hotels directly to arrange for accommodations. Since many of these are located in historic buildings, not all rooms are provided with in-room wi-fi and/or A/C, even in high-end hotels. If either of these is important to you, please check with the hotel at the time of making your reservation. The weather in Morelia in early April is warm and dry, with highs ~ 28 C (82 F) and lows ~ 13 C (55 F).
Two hotels offer special rates for conference participants. To obtain the special rate it is necessary to make the reservation by email or telephone mentioning the code MSSF17. Not applicable for online reservations.
Hotel Misión Catedral (ventascatedralmorelia@hotelesmision.com.mx)
Hotel Alameda (lcchora@hotel-alameda.com.mx)
We provide a list of restaurants in downtown of city, some of them offering vegetarian options (**)
The early registration fee for the conference is $180 USD ($150 USD for students) due before January 31st, 2017. After that, the registration fee is $250 USD ($180 USD for students). There is the possibility that we will be able to provide financial support for a limited number of students and young researchers.
The registration fee for participants from Mexican institutions is payable in Mexican pesos. The early registration fee is $3,240 MXN ($2,700 MXN for students). After January 31st, the registration fee is $4,500 MXN ($3,250 MXN for students).
Payment MUST be made via bank transfer since we will be unable to receive any payments at the registration desk. In all cases, please send us a copy of the transfer invoice at your earliest convenience.
IMPORTANT NOTICE FOR PARTICIPANTS FROM UNAM: La UNAM no genera facturas para sí misma, por lo que sólo podemos entregar un recibo normal o un CFDI como persona física.
For deposits in the bank:
Send an email to: d.garcia@crya.unam.mx
We will return specific information for deposit in bank.
For transferences ONLY:
Universidad Nacional Autonoma de Mexico
Bank: BBVA Bancomer
Account number: 0446634494
CLABE interbancaria: 012180004466344942
Concept: IRYA UNAM MSSF 17
(Participant's name, and institution).
Universidad Nacional Autonoma de Mexico
Bank: J.P. Morgan Chase Bank N.A.
Account number: 00101693118 (DLLS)
Swift Code: CHASUS33
Address: Texas Market P O BOX 659754
San Antonio, TX 78265-9754
Concept: IRYA UNAM MSSF 17
(Participant's name, country of origin, and institution).
Universidad Nacional Autonoma de Mexico
Bank: J.P. Morgan Chase Bank N.A.
Account number: 00101693118 (DLLS)
Swift Code: CHASUS33
ABA US transfer: 111000614
ABA Europe transfer: 21000021
Address: Texas Market P O BOX 659754
San Antonio, TX 78265-9754
Concept: IRYA UNAM MSSF 17
(Participant's name, country of origin, and institution).
Please indicate whether you have paid also for the conference dinner ($50 USD / $900 MXN) and the tour ($30 USD / $540 MXN) in the corresponding boxes. Dinner are planned for Tuesday April 4th and the tour Wednesday April 5th.
* Rates in Mexican pesos apply to participants from Mexican institutions only.
Download Program PDF
Download Abstracts PDF
WARNING: This is not a final version of the Program/Abstracts book.
Please consider download again a new version of the PDF during the event.
The poster dimensions should not exceed the A0 format (118 by 84 cm, or 46.8 by 33.1 in) in portrait mode.
Posters will be assigned a code depending on range of scales: large (L), medium (M), small (S); and a number, such as in S20. The final poster program will be posted here soon, as well as an option to upload it in case the author desires to give a 1 minute presentation of it.
CODE | AUTHOR | TITLE |
---|---|---|
PS01 | Isequilla, N | Radio observations of evaporating in the Cygnus OB2 region |
PS02 | Gómez Maqueo Chew, Y | Fundamental properties of the eclipsing pre-main sequence components of MML 53 |
PS03 | Koutoulaki, M | AMBER/VLTI Medium spectral resolution observations of the Bracket gamma and high-n Pfund emitting regions of the Herbig B[e] star HD50138 |
PS04 | Shan, Y | Multiplicity of Pre-Main Sequence M-dwarfs in Young Moving Groups (YMGs) |
PS05 | Guszejnov, D | Consequences of Scale Free Fragmentation in Star Formation |
PS06 | Masqué, J | Searching for compact radio sources associated to UCHII regions |
PS07 | Paron, S | Multi-scale and multi-wavelength study of the UCHII G45.47+0.05 surroundings |
PS08 | Kee, N | The Role of Line-Driven Outflows in the Formation of Massive Protostars |
PS09 | Sanna, A | Gas dynamics driven by an O-type YSO: from 0.1 pc down to 100 AU |
PS10 | Sánchez-Monge, A | An ALMA view of SgrB2: continuum characterization and spectral line survey |
PS11 | Cappa, C | Star formation, gas and dust in the IR dust bubbles complex S21-S24 |
PS12 | Fedriani, R | Kinematical and Dynamical Study of IRAS 13481-6124 primary jet |
PS13 | Ahmadi, A | CORE: A NOEMA large program to investigate fragmentation and disk kinematics during high-mass star formation |
PS14 | Ortega, M | Misaligned molecular outflows and precessing jet towards the massive young stellar object G034.5964-01.0292 |
PS15 | Kumar, N | O-star binary systems in formation |
PS16 | Hernández, J | A large scale survey of Herbig Ae/Be stars in the Orion Star Forming Complex - GAIA view |
PS17 | Frimann, S | Large-scale numerical simulations of star formation put to the test. Comparing synthetic images and actual observations for statistical samples of protostars. |
PS18 | Camacho, V | Energy budget of forming clumps in numerical simulations of collapsing clouds |
PS19 | Feddersen, J | Probing a molecular cloud from 0.01 to 10 pc scales: The CARMA Orion Survey |
PS20 | Sandell, G | SOFIA, a unique observatory for studying star formation process |
PS21 | Sandell, G | NGC7538 IRS1 & South – our key to understanding high mass star formation |
PS22 | Rodríguez-Kamenetzky, A | Non-Thermal Emission From Protostellar Jets |
PS23 | Hernández-Gómez, A | VLA centimetric observations towards IRAS16293-2422 |
PS24 | Gómez-Ruiz, A | Polarization structure of protostellar shocks |
PS25 | Nony, T | High-mass star formation in the W43-MM1 protocluster |
PS26 | Sierra, A | Dust emission of protoplanetary disks |
PS27 | Suárez, G | Towards a complete study of the initial mass function and early kinematics evolution of the 25 Orionis stellar group |
PS28 | Kölligan, A | Jets and Outflows of Massive Protostars |
PS29 | Manzo-Martínez, E | Evolutionary models of accretion disks: IR emission and snowlines evolution |
PS30 | Lopez-Vázquez, A | Angular momentum in bipolar outflows |
PS31 | Sewilo, M | The Very Large Array ammonia observations of the HH 111/HH 121 protostellar system: a detection of a new source with a peculiar chemistry |
PS32 | Treviño-Morales | Deuteration around the ultracompact HII region Mon R2 |
PS33 | Liao, L.-W. | A bipolar molecular jet in NGC2023 MM1 |
PS34 | Rojas, S | Searching for collimated outflows candidates in massive star-forming regions |
PS35 | Tapia, M | A new infrared view of the NGC 6634-V region |
PS36 | Tapia-Schiavón, L | The heating efficiency and the star formation rate in very young stellar clusters |
PS37 | Ferrero, L | Southern hemisphere jets and molecular outflows observed with Gemini and APEX: the case of HH 137 and HH 138 |
PS38 | Rodríguez-Garza, C | A survey of 44-GHz Class I methanol masers toward High Mass Protostellar Objects |
PS39 | Rodríguez-Garza, C | Early science with the Large Millimeter Telescope: a 3 mm spectral line survey of massive protostars with class I methanol masers |
PS40 | Ramírez, V | Kinematics of Cromospherically Active Stars in the RAVE Catalog |
PS41 | Naranjo-Romero, R | Hierarchical gravitational fragmentation. I. Collapsing cores within collapsing clouds |
PS42 | Orozco, T | Molecular study of two inter-mediate mass hot cores in OMC1 |
PS43 | Rangaswamy, D | Near-Infrared Polarimetry of the S235 star-forming complex |
PS44 | Zamora, M | The magnetic field as a turbulence suppressor in molecular cloud formation |
PS45 | Toalá, J | A young Hot Bubble within the HII region SMC-N88 |
PS46 | Rodgers-Lee, D | Low energy protostellar cosmic rays in protoplanetary disks |
PS47 | Zepeda, D | LMT study of 1.1mm cores in Orion A molecular cloud |
PS48 | Slepian, Z | Collapse of spherical cores embedded in a low-density filament: analytic predictions |
PS49 | Jung, M | First light emerging from the clouds |
PS50 | Zhang, Han | Constraining the magnetic fields in Young Stellar Objects (YSOs) |
PS51 | Binks, A | Improving ages for nearby, young moving groups |
PS52 | Lee, Y | |
PS53 | Castañeda, H | |
PS54 | Luna, A |
CODE | AUTHOR | TITLE |
---|---|---|
PM01 | Barnes, A | Star formation rates and efficiencies in the Galactic Centre |
PM02 | Ramón-Fox, G | Exploring the role of large scale flows in molecular cloud formation in spiral galaxies |
PM03 | Dzib, S | The GLOSTAR VLA Galactic plane survey |
PM04 | Rugel, M | OH gas properties and feedback in the Milky Way as seen in the THOR survey |
PM05 | Medina, S | Turbulence Analysis on Galactic Plane Molecular Clouds |
PM06 | Armentrout, W | Star Formation Efficiency in the Outer Scutum-Centaurus Arm |
PM07 | Kendrew, S | Tracing massive stellar feedback in the Milky Way Galaxy |
PM08 | Colombo, D | Building a (fully resolved) molecular cloud catalog of the Milky Way |
PM09 | Fissel, L | Magnetic Fields in Star Formation: A Detailed BLASTPol Study of the Vela C Giant Molecular Cloud |
PM10 | de la Fuente, D | Early evolution of stellar populations in a giant star-forming complex: the Dragonfish nebula |
PM11 | Hernández, Audra | A Catalog of the Southern Molecular Cloud Physical Properties from the ThrUMMS Survey |
PM12 | Anderson, L | The Galactic Distribution of High-Mass Star Formation Regions |
PM13 | Rendón, J | Insufficient Reservoirs of Molecular Gas to Form a Second Stellar Population in LMC Massive Star Clusters |
PM14 | Rodríguez, Jimena | Systematic study of young star clusters in the galaxy NGC 253 |
PM15 | Smilgys, R | Formation of stellar clusters in galactic spiral arms |
PM16 | Pitts, R | Continuum Emission Diagnostics for Pretsellar Clumps in the CHaMP Survey |
PM17 | Towner, A | Mid-IR and Centimeter Observations of 20 High-Mass Protoclusters in the Milky Way |
PM18 | Alzate, J | Stellar population parameters of the Milky Way Galaxy and photometric detection of satellite galaxy remnants |
PM19 | Lucas, P | Highly variable protostars from the UKIDSS Galactic Plane Survey |
PM20 | Vavrek, R | boloSource() for the analysis of diffuse emission and crowded-field photometry |
PM21 | Peñaloza, C | Using synthetic observations to constrain the evolution high tracers in molecular clouds |
CODE | AUTHOR | TITLE |
---|---|---|
PL01 | Vega-Acevedo, I | Star formation efficiency in tidal tails of mergers |
PL02 | Pellegrini, E | Beyond the Peak Spatially resolved CO Excitation in the Local Universe |
PL03 | Méndez-Hernández, H | Probing the circum-galactic gas with VUDS |
PL04 | Obi, Ikechukwu | SEDs of nearby star-forming galaxies with the new PARSEC evolutionary tracks: Star formation rates and Dust Attenuation Properties |
PL05 | Esparza-Arredondo, D | Coevolution between multiscale star-formation and AGN activity |
PL06 | Hidalgo-Gámez, A | The SFR of compact, coloured galaxies |
PL07 | Magaña-Serrano, M | Calibrando la tasa de formación estelar en Hα y FUV para galaxias tardías |
PL08 | Ramírez-Siordia, V | Deriving the Star Formation History of Stellar Systems Containing Few Stars |
PL09 | Elías-Chávez, M | Estimation of the star formation rate through data analysis of SWIFT's long GRBs from 2008 to 2016 |
PL10 | Calvi, R | The morphological dependences of SFR-mass relations for local star-forming galaxies in different environments star-forming galaxies in different environments |
PL11 | López-Cobá, C | Star-formation driven galactic winds in UGC 10043 |
PL12 | González-Samaniego, A | Star formation and mass estimators in dwarfs galaxies vs. cosmological simulations |
PL13 | Arrabal Haro, P | High-z Ly_alpha sources search using the SHARDS survey |
PL14 | Boquien, M | |
PL15 | Hart, R | |
PL16 | Pappalardo, C |