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Discussion Summary, "Philadelphia, the Place that Loves You Back"
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Following opening remarks by Encyclopedia of Greater Philadelphia co-editor Howard Gillette, roundtable facilitator and fellow co-editor Charlene Mires (Mid-Atlantic Regional Center for the Humanities at Rutgers-Camden) introduced the panelists and discussion topic, "Philadelphia, the Place that Loves You Back." Mires reflected on the history of tourism, specifically tourism's role in shaping how Philadelphians and visitors alike view the city and region. To this point, Mires called attention to the site of the evening's discussion, the Independence Visitor Center, as well as the surrounding historic sites, museums, and landscapes as evidence of the city's investment in visitor services and its desire to attract them. Mires then transitioned to a brief history of the term "tourism," meaning "to travel for pleasure," which came into use in the early nineteenth century. Noting that tourism first carried negative connotations, Mires speculated that, in an era marked by democracy, industrialization, and turmoil, tourism was viewed as perhaps too self-indulgent and elitist. Notably, the rise of tourism coincided with Philadelphia's loss of national prominence, yet the city's history and reputation as "the Quaker City," "the City of Brotherly Love," "the Cradle of Liberty," and "the Athens of America" still attracted tourists to the city.
Interestingly, when visitors came to Philadelphia in the 1800s, Mires observed that they primarily came to see what was new, from Eastern State Penitentiary and the Fairmount Waterworks to Girard College. Mires described how tourists also participated in the city's living history by attending church services, observing trials, and visiting hospital wards, as well as taking in the surrounding countryside both on the Wissahickon and Fairmount Park. Additionally, while some visited historic sites like Independence Hall and the Liberty Bell, Mires noted that, until its steeple was reconstructed in 1828, Independence Hall was not a major attraction and the Liberty Bell did not gain fame as an icon until the 1830s and 1840s. Over time, Philadelphia's new attractions of the nineteenth century became the historic attractions of today and Mires asserted that it is these intersections of old and new that make the history of tourism in Philadelphia especially interesting.
As Mires explained, the conflict between old and new was exemplified by the 1876 Centennial, which celebrated the anniversary of the Declaration of Independence with a world's fair showing off the latest in arts and industry; Mires observed that such tensions persist into the twentieth century and beyond, as Philadelphia's promoters have struggled to market the city as more than a sleepy town of old brick buildings. Mires concluded her remarks by referencing panelist Richardson Dilworth's essay "Philadelphia, the Place that Loves You Back," which was published in the Philadelphia Inquirer and on the Encyclopedia of Greater Philadelphia website prior to the roundtable. Mires identified Dilworth's essay as a starting point for the evening discussion and invited the panelists to recall a personal tourist experience and offer their perspective on tourism in Philadelphia.
The first panelist, Richardson Dilworth (Drexel University), began his comments by reminiscing about growing up in Society Hill and admitting that, at the time, he did not think about tourists visiting the sites around his neighborhood. Dilworth then reflected on the inspiration for the evening's discussion, the popular 1990s tourism slogan "Philadelphia, the Place that Loves You Back." Dilworth observed that, while he was not living in Philadelphia when the slogan was in use, he felt its power and impact because the slogan extended beyond Philadelphia and stuck with him. Dilworth also argued that the slogan's power can be partly attributed to the confusion and questions it provoked, such as "how can a place experience emotion?" and "why is Philadelphia 'the place that love you back?'"
Dilworth described Philadelphia's prevailing reputation prior to the 1990s as antisocial, a reputation that, in his view, arose from the Quaker values of tolerance and acceptance. As Dilworth later explained, tolerance requires indifference and Philadelphia's antisocial reputation is intimately tied to its perceived virtues to the extent that it is a point of pride for Philadelphians. Dilworth concluded by observing that, while cities do not have agency in the way individuals do, it is difficult to deny that agency is often assigned to cities and take on weight and meaning in the cultural imagination, as demonstrated by the success of "Philadelphia, the Place that Love You Back."
By way of introduction, the second panelist, Meryl Levitz (Greater Philadelphia Marketing Corporation), shared her early experiences of Philadelphia, specifically her decision to move to the region in the 1970s. Levitz related how, as she and husband listed places they would and would not want to live, they somehow neglected to include Philadelphia and wondered what this oversight said about their perceptions of the city. However, after visiting Philadelphia and getting lost in its neighborhoods, Levitz developed affection for the city and, now commuting from New Jersey to Philadelphia, Levitz observed that she enters the city everyday as a tourist.
The third panelist, Bob Skiba (Association of Philadelphia Tour Guides), focused his comments on his role as a tour guide and the relationship between how residents and tourists view the city. As Skiba contended, the image that Philadelphia projects to visitors is intimately tied to how residents see the city and make it a viable place to live through arts, culture, restaurants, and political debate. Among American cities, Skiba also made the point that Philadelphia is perhaps most closely tied to its founder and described William Penn as a tourist who marketed Philadelphia to attract other settlers. By virtue of Penn's promotion of the region's fertile soil, restaurants and pubs, religious freedom, and economic success, Skiba observed that Philadelphia was the largest city in America at the time of independence and subsequently continued to attract attention and tourists, including 10 million visitors for the 1876 Centennial. Reflecting on Philadelphia's sense of self, Skiba remarked that, in his twelve years as a tour guide, he has seen the city become more energetic, welcoming, and self-confident, as Philadelphians increasingly project a love of the city that they share with visitors.
Following the panelists' opening remarks, Charlene Mires posed a question to the speakers: What do tourism promotions communicate about the city and region? Responding first, Meryl Levitz spoke about crafting the "Philadelphia, the Place that Loves You Back" slogan in the 1990s. Levitz related how every word was chosen carefully and that, similar to Nike's "Just Do It" tagline, the slogan was initially met with questions about its meaning. In terms of the slogan's development, Levitz described how, amidst Philadelphia's industrial decline, hospitality was targeted as an industry with the potential to replace the city's lost manufacturing base; however, as Levitz noted, in order to become a prime tourist destination, Philadelphia needed not only a new tourist center, but also a psychic overhaul to combat Philadelphians' dismissive attitude about their own city.
To this end, the Greater Philadelphia Marketing Corporation (GPMC) struggled with several slogans, such as "Philly Plus: Bigger Than the Bell," "Philadelphia: Town and Country," and "Find Your Philadelphia," before settling on one that played off such successful taglines as "Virginia is for Lovers" and "I Love New York." By emphasizing the relationship between person and place, Levitz explained how the GPTMC consciously avoided comparisons to other cities and crafted a slogan that personified Philadelphia and implied a mutual affection. Levitz also reflected on several other strategies behind the slogan, such as the choice of "Philadelphia" over "Philly" (the latter implying an affection that people didn't feel) and the decision to market the slogan to residents and visitors alike.
Bob Skiba followed Levitz's remarks by noting that he liked the slogan, particularly the way it anthropomorphized the city. Echoing his earlier remarks, Skiba stated his view that tourists' experiences are largely about the people they interact with, and "Philadelphia, the Place that Loves You Back" further humanizes the city. Richardson Dilworth concurred and described an ongoing trend to attribute human characteristics to cities; to this point, Dilworth specifically related how the unification of the five boroughs of New York City was described as a "forced marriage" between Manhattan and Brooklyn. Responding to the panelists' comments, Charlene Mires observed that slogans are about both place and personality and alluded to Philip Stevick's Imagining Philadelphia: Travelers' Views of the City from 1800 to the Present, an analysis of how tourists described their experiences visiting Philadelphia.
Mires then posed another question to the panelists: How are Philadelphia's historic places both an asset and a challenge for promoting the city to today's visitors? Bob Skiba observed that Mires' question captured the disjuncture between a historic and living city and remarked that the entire city of Philadelphia is in fact a historic area. Meryl Levitz followed Skiba's comments by relating a memorable encounter during 1993's "Welcome America" events, when a tourist couple wondered why historic Fort Mifflin had been built so close to the airport. This illustrated Levitz's contention that visitors don't expect things to be real and that, to best communicate with visitors, we must talk in current terms while also showing that Philadelphia is the real deal. Levitz also emphasized the need to keep historic sites clean and attractive through the use of window boxes and green space.
Richardson Dilworth reiterated that tensions exist between Philadelphia's tradition of tolerance and its accompanying antisocial reputation and efforts to be open and inviting to visitors. As Dilworth detailed, to achieve greater intimacy and a stronger sense of community, cities must give up some of their tolerance of difference, a phenomenon chronicled in Jane Jacobs' The Death and Life of Great American Cities.
Following the panelists' remarks, Charles Mires opened the discussion to questions from the audience. The first question came from an audience member who commented about the need for money as well as slogans to promote tourism and asked about opportunities for various local organizations to pool their resources to market Philadelphia to visitors. Meryl Levitz responded that, in light of cuts in state tourism funding, cooperation is a necessity and detailed how Philadelphia's tourism marketing budget pales in comparison to such destinations as Las Vegas and Orlando. Levitz also shared how the GPTMC's newest marketing campaign, "With Art, Philadelphia," is a collaboration of visual artists and visual arts organizations. News of this collaboration prompted several follow-up questions, as one attendee asked about opportunities for bringing together makers and preservers of art and another inquired about efforts to connect Philadelphia's neighborhoods to Center City and the historic district. Levitz reiterated that such personal and neighborhood connections are the goal of the "With Art, Philadelphia" campaign and expressed a desire to tap into the energy of the artistic community.
Other audience questions focused on efforts to increase tourism, whether through marketing, visitor resources, or streamlining travel between other cities and nations. In response to a question about boosting the number of European tourists, Meryl Levitz related that, while the Internet has been a great boon for attracting visitors from abroad, international visitors to Philadelphia still number in the hundreds of thousands, not the millions. Levitz explained that the cost of a good consumer tourism campaign is about $3 million per country and that, even with emerging markets like India, Brazil, and China, the need for better airports and direct flights hampers the growth of international tourism to the city. Bob Skiba commented that, as a tour guide, his contact with international visitors has increased from year to year and suggested that a cell phone app for European tourists would be especially useful. Following a question about resources for planning tourism excursions and travel restrictions between New York and Philadelphia, Meryl Levitz also remarked on the growth of Bolt and Mega Bus and detailed resources like visitphilly.com, which includes itineraries for families.
The question and answer session concluded with some comments about images of Philadelphia in popular culture. One audience member inquired about the source of Philadelphia's apologetic nature and proposed that promising not to hate Philadelphia might be a good starting point for a new tourism slogan. The last question of the evening focused on the positive and negative effects of depictions of Philadelphia in television and movies. In response, Meryl Levitz detailed the GPTMC's crusade against the popular television show "Parking Wars" and the number of e-mails they receive from people who vow not to visit Philadelphia based upon what they see on the show. In contrast, Levitz noted that shows like "It's Always Sunny in Philadelphia" cast the city in a popular light and appealed to popular culture to focus on happy topics involving Philadelphia. Following the question and answer session, the evening ended with small group discussions in which audience members shared additional comments and proposed topics for the Encyclopedia of Greater Philadelphia.
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By Love Letters to Philadelphia: Gendering an urban brand | History@Work on June 20, 2012 at 4:31 am
[…] corner adds the specificity of place that the original lacks. [3] Dilworth made this point during a public discussion of tourism as part of the Encyclopedia of Greater Philadelphia. [4] Steve Macek. Urban Nightmares: The Media, […]


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Q: Combination/Permutation understanding check I have a (fairly) simple combination and permutation question, but I'm prone to silly errors and I want to make sure this looks good! I'm a little stuck on D) so direction would be nice :)
Given an alphabet of 13 uppercase letters (N-Z), how many 7 letter strings are there if:
A) No letters can be repeated? Permute(13,7) = 8,648,640
B) Letters can be repeated? $13^7$ = 62,748,517
C) Letter can not be repeated and start with either 'Z' 'U' or 'X'?
Perm(12,6) + Perm(12,6) + Perm(12,6) = 665,280
D) Letters can be repeated and at least on one the following conditions is true.
(i) String starts with Z (ii)fourth letter is U (iii)String ends with x
P(12,6) + P(12,6) + P(12,6) - the overlap of the three (but how?!)

A: A, B and C are correct.
For D, $P(12,6)+P(12,6)+P(12,6)$ is a good start. The problem is that words like Z__U___ are counted twice, so you should subtract those out. Same for Z_____X and ___U__X. So far, we are at
$$
P(12,6)+P(12,6)+P(12,6)-P(11,5)-P(11,5)-P(11,5)
$$
Now, every word has been counted the appropriate number of times except for Z__U__X. Words like this were initially triple counted, but after the first adjustment they were also subtracted out three times, and are no longer counted at all. Therefore, they need to be added back in, for a final answer of
$$
P(12,6)+P(12,6)+P(12,6)-P(11,5)-P(11,5)-P(11,5)+P(10,4)
$$

redpajama_set_name: RedPajamaStackExchange


The Wetumpka Fire Department is an ISO rated Class 4 fire department that provides services to over 20,000 residents within a 70 square mile coverage area in around the City of Wetumpka. The department utilizes a combination of volunteer, part-time and full-time personnel to provide fire, EMS, and rescue services from 4 stations strategically located throughout the fire district. Our apparatus fleet includes 4 engine companies, 1 medium rescue, 1 ladder company, 1 tanker/pumper, 3 brush units, and 1 command vehicle as well as 6 boats and other dive and technical rescue trailers. The department emphasizes public education, training and planning to ensure that our citizens and visitors are provided with the best services possible.
Our public education program focuses on the more than 3000 children who not only live within our fire district but also arrive from 7 other fire districts to attend our local schools. Recently, our public education program has received recognition in national fire service periodicals such as Firehouse, Fire Engineering, Fire Chief, the NFPA Journal and others for our education efforts in the area of fire sprinklers.
Our dedication to training is evidenced by many of our personnel acquiring advanced certifications as instructors, inspectors and fire officers and also by the many technical certifications required to participate in our dive, swift-water and high-angle teams.
Planning is an obvious priority of our department as a result of potential hazards such as our large school population, many government buildings, Tutwiler Prison, Jordan Dam, Elmore Community Hospital, the Coosa River, US Highway 231, historic downtown riverfront area and the Wetumpka Airport. Additionally, the City attracts many tourists and host many events that draw large crowds to our fire district.
The department participates in the Elmore County Firefighter�s Association, works closely with the Elmore County Emergency Management Agency and has mutual aid agreements with surrounding departments in the county, particularly the neighboring fire districts of Elmore, Holtville, Titus, Byuck, Santuck, Eclectic, Emerald Mountain, and Redland.


This disc is a standout, with terrific performances and a compelling program of works, all confronting the relationship between the past and the present.
In Kammermusik No.3 from 1925, German composer Paul Hindemith looks back to the Baroque, especially to Bach's Brandenburg Concertos. The Vancouver-based Turning Point Ensemble, under Owen Underhill's direction, handles the inventive contrapuntal textures with stylish buoyancy, while Canadian cellist Ariel Barnes brings out Hindemith's lyrical side. Barnes' restraint with vibrato and Romantic phrasing is especially appropriate to Hindemith, an accomplished violist who was deeply involved in historical performance practices.
At the same time that avant-garde Italian composer Luciano Berio was creating his pioneering experimental works like Sinfonia, he was working on arrangements – and rearrangements – of music of the past, from Monteverdi to Puccini. In Folk Songs, from 1964, he creates altogether new accompaniments for traditional folk tunes (plus a few composed songs) from around the world. The result is an extraordinary mélange of styles and harmonic languages. Canadian vocalist Fides Krucker's blazing theatricality and playful brilliance put her in the same league as the fabulous American singer Cathy Berberian, who premiered this work.
Canadian composer and conductor Underhill's own Cello Concerto from 2016 takes us through the fragmentation and reassembling of memories of the past, triggered by a Chinese curio box full of precious objects. The virtuosic, responsive Turning Point Ensemble under Underhill's precise direction creates evocative, colourful interplay with Barnes' adventurous and dramatic cello playing.
I enjoyed the anecdotal liner notes and bios, but I do wish there were texts for the songs – with translations.


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Peacing Together: The benefits of clearing your record and how to do it
Finding a job isn't always easy, and a criminal record doesn't make it any easier
Author: Amyre Makupson
Published: 5:46 PM EST January 30, 2020
Updated: 5:46 PM EST January 30, 2020
MACON, Ga. — Through our partnership with Mercer University's Center for Collaborative Journalism, as part of our Peacing Together series, we're looking at youth violence and ways to stop it.
Amyre Makupson has more on how local government and law enforcement are working to get Maconites behind a desk working, so that they won't be behind jail walls serving time.
BACKGROUND: Peacing Together: Seeking solutions to youth violence in Central Georgia
"I think young people, once they receive a felony on their record, they think their life is over, but their life is not over," said Macon-Bibb commissioner Al Tillman.
Tilman says everyone makes mistakes, especially youth, but a mistake that results in a criminal record can have lasting impact for years to come.
That is why county leaders are trying to get the word out about record expungement.
"Things don't fall off in Georgia," said Andrew Feagan. He's the assistant Public Defender at Macon-Bibb County Public Defender's Office
He says criminal offenses can live on your record unless you have them expunged or removed.
"The most typical things that can be restricted on your record would be if you were arrested for something and for whatever reason you weren't prosecuted, those dismissals, things where the statute of limitations have run," he said.
And once you have a clean slate, you're more attractive to potential employers.
"We have so many positions for everybody. We have full time positions, we have part time positions," said Spectra general manager David Aiello.
Aiello manages the Macon Centreplex and Macon City Auditorium, and he says Spectra is more concerned with your mindset now than what you did when you were younger.
"We're looking for someone that's going to come in, be a hard worker that's going to take direction and then we can find a fit for everybody," said Aiello.
Because everyone deserves a second chance at a better life.
"They can at least come to the table and talk to the employer and say, hey, I'm married now, I've gone to school, I've changed my life. That happened 15-20 years ago. Where in years past, if you had to say yes, I'm a convicted felon, your application would probably get thrown in the trash," said Tillman.
To find out if you qualify to have your record expunged, the public defender's office in downtown Macon will meet with you for free.
You may have to pay some fees to file the paperwork. You will also have to bring a copy of your criminal record with you.
The phone number for the Public Defender's Office is 478-621-5950. The office is located at 201 Second Street (#550) in downtown Macon.
You can get your criminal record from the Bibb County Sheriff's Office by calling 478-751-7500.
Five years ago, Governor Nathan Deal signed a Georgia law banning the criminal history question on job resumes. President Obama later signed a "Ban the Box" executive order that covers federal hiring.
MORE PEACING TOGETHER
Peacing Together: Bibb school counselors train to identify students' emotional needs
Peacing Together: Pilot program at Bibb schools teaches mindful breathing to boost self-control
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Have a news tip? Email news@13wmaz.com, or visit our Facebook page.

redpajama_set_name: RedPajamaCommonCrawl


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\section{Introduction}
The early Universe was $\alpha$-enriched because type II supernovae (SNe II) occurred on a much faster time-scale than type Ia supernovae (SNe Ia), and whereas the former produce a great amount of $\alpha$-elements and less iron, the latter are the main production sites of Fe-peak elements \citep[e.g.][]{edvardsson1993}. And so iron-group elements found their way to the interstellar medium (ISM) much later than those formed by $\alpha$-captures. With this in mind, the ratio of $\alpha$-elements over iron ([$\alpha$/Fe]) against metallicity can be interpreted as a cosmic clock depicting some aspects of the Galactic chemical evolution \citep[GCE,][]{haywood2013, buder2018, dmena2019}.

Sulfur is an $\alpha$-element produced in SNe II by hydrostatic and explosive burning of oxygen and silicon \citep{woosleyweaver1995, fenner2004}. For long, it was a neglected element in the study of GCE due to the large uncertainties associated with its derivation, and so other $\alpha$-elements were preferred, such as Si and Ca, which have similar nucleosynthesis. Be that as it may, sulfur is a volatile element, and as such, does not form dust grains in the ISM \citep{savagesembach1996}, making it an ideal depletion-independent tracer of the evolution of galaxies.

In the early 2000s, different trends were reported with regard to the evolution of sulfur. They all agreed that \sfe\ was solar around \mbox{\feh\ $=0$} dex and increased with decreasing metallicity, down to \mbox{\feh\ $=-1.0$} dex. However, in the metal-poor regime, the findings did not reach a consensus. Earlier studies found \sfe\ ratios rising up to $\sim$0.8 dex \citep{israelian2001, takada-hidai2002} or a bimodal behaviour with both high ratios and ratios on a plateau at $\sim$0.3 dex \citep{caffau2005}, but a majority of authors proposed an $\alpha$-like behaviour, showing only ratios on a plateau around 0.3 dex \citep[e.g.][]{chen2002, ryde2004}. This trend has been confirmed by most recent studies \citep[e.g.][and references therein]{duffau2017, caffau2019}.

In terms of the elemental abundances of the Milky Way's populations, it has been found that $\alpha$-elements are more abundant in the thick disk rather than the thin disk \cite[e.g.][]{navarro2011, adibekyan2011, bensby2014}. However, analysis into how sulfur abundances are distributed according to Galactic populations are scarce, thus we aim to analyse if sulfur shows a Galactic distribution similar to that of other $\alpha$-elements by using the HARPS-GTO sample.

Additionally, sulfur is also considered an important building block of terrestrial planets, alongside Fe, Mg, Si, C, and O \citep{bond2010}. It is present in the core of rocky planets, usually in the form of iron alloy, e.g. FeS, and possibly in the mantle, although in smaller amounts \citep{brugger2017, santerne2018, wang2019}. Recent studies \citep{dorn2015, santos2015} into the composition and internal structure of terrestrial planets have concluded that host stellar abundances can be used to set additional constraints when modelling the interiors of these planets, helping to reduce the degeneracies of the models. The planet bulk abundance can generally be assumed to be the same as the star for refractory elements, but not for volatile elements, such as sulfur, carbon or oxygen. In these cases, as the planet is devolatilised, the extent of volatile depletion has to be estimated according to distance from the star and the bulk abundances of the planet can then be inferred from the host stellar abundances \citep[see][and references within]{wang2019}.

This paper is a continuation of the work started by \citet[][hereafter A12]{adibekyan2012a} and followed by \citet[][hereafter DM17]{dmena2017}, where precise chemical abundances were derived for more than 1000 stars in the solar neighbourhood, although we employ spectral synthesis to fit observational spectra instead of the Equivalent Widths technique. It is structured in the following way: in Section 2, we will characterise the sample and the stellar parameters; Section 3 describes the process of deriving sulfur abundances and the associated uncertainties; in Section 4, we present and discuss our results in the context of GCE, compare them to theoretical models and study the differences in sulfur abundances between planet hosting and non-planet hosting stars; finally, Section 5 will summarise our conclusions.

\section{Sample description and stellar parameters}

The original sample was composed of 1111 FGK stars observed in the context of three HARPS-GTO planet search programs \citep{mayor2003, locurto2010, santos2011}. The majority of the stars are slow rotators, non-evolved, and have low chromospheric activity levels. The individual spectra of each star were reduced using the HARPS pipeline and then combined with IRAF\footnote{IRAF is distributed by National Optical Astronomy Observatories, operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation, USA.} after correcting for its radial velocity shift. The resolution is $\sim$115 000 and the signal-to-noise ratios (S/N) range from $\sim$20 to $\sim$2000, although most of the sample has high S/N (85\% of the sample has S/N higher than 100).

Stellar parameters were derived in a homogeneous way for the entire sample in \citet{sousa2008, sousa2011a, sousa2011b}. Later, the parameters for cooler stars (\teff $<$ 5200 K) were re-determined \citep[][DM17]{tsantaki2013} using a reduced list of iron lines specially assembled to avoid blending effects. DM17 also corrected the spectroscopic gravities (\logg) of the sample. Abundance references were derived from a solar reflected light spectrum of the Vesta asteroid, also obtained with the HARPS spectrograph. For further details on the sample and parameter determination, see A12 and DM17.

The final result was a sample of 1059 solar neighbourhood stars, with effective temperatures from 4393 K to 7212 K (98\% of the stars have \mbox{4500 K $<$ \teff $<$ 6500 K}), surface gravities from 2.75 to 5.06 dex (96\% stars have \mbox{4 $<$ \logg $<$ 5 dex}), and metallicities ranging from -1.39 to 0.55 dex. This sample contains 150 planet hosts (29 Neptunian-mass planets or Super-Earths and 121 Jupiter-like planets) and 909 stars which are not known to harbour any planetary companions\footnote{Due to the HARPS radial velocity precision and the long-term duration of the survey, we can only be sure that these stars do not host giant planets. However, we cannot guarantee that they are not hosts to smaller planets, specially those with long periods.}.

Chemical abundances of other elements have been derived in an homogeneous way for this sample by other authors: refractory elements \mbox{\textit{A}$<$29} (A12), lithium \citep{dmena2014, dmena2015}, carbon \citep{sandres2017}, oxygen \citep{bdlis2015}, and neutron capture elements (DM17). Additionally, for a fraction of the stars in this sample, beryllium abundances can be found in \citet{santos2004a, galvez-ortiz2011, dmena2011, dmena2012} and nitrogen abundances in \citet{sandres2016}.

\section{Derivation of chemical abundances}
Synthetic spectra were created assuming local thermodynamic equilibrium (LTE) using the 2017 version of the spectral synthesis code MOOG \citep{sneden1973}, with the driver \textit{synth}. The stellar atmospheres models are from \citet{kurucz1993}, being the same ones used to derive stellar parameters and other elements' abundances. The line lists for the spectral regions were taken from VALD \citep{kupka-ryabchikova1999}, although the atomic parameters of some lines had to be slightly changed to better match the solar spectra (see more in Section 3.2).

\subsection{Rotational velocity and macroturbulence}
The values of rotational projected velocity (\vsini) and macroturbulence (\vmac) of the stars are inputs required by the MOOG code as they take part in the broadening of the atomic lines, so in order to derive sulfur abundances, we first had to compute these two parameters.

Macroturbulence values for stars in the temperature range of 5000K to 6500K were determined with Equation (8) from \citet{doyle2014}, which is a temperature and gravity dependent formula. Stars with temperature below 5000K were assigned a value of 2.0\kms\ and for those above 6500K, \vmac\ was set to 5.5\kms.

As for the rotational velocity, we produced synthetic spectra with MOOG (using the previously derived \vmac\ value) and fitted it to the observed spectra in 36 wavelength regions where over 70 FeI and FeII lines are present. We used the Python package \mbox{\textit{mpfit}} \citep{markwardt2009} to find the best fit and corresponding \vsini\ value by fixing the \feh\ abundances and all other stellar parameters and setting \vsini\ as the only free parameter. The package performs $\chi^2$ minimisation of the deviation between the synthetic and observed data sets in order to find the best-fitting values of the free parameter defined by the user. Errors are automatically computed by the package as well.

For ten stars in our sample (HD82342, HD55, HD108564, HD145417, HD134440, HD23249, HD40105, HD92588, HD31128, HD52449), the value of \vmac\ that was first attributed to them caused a malfunction in the code that determined \vsini, possibly due to \vmac\ being too large a value, as it tried to compensate by finding \vsini\ values that were below 0.1 \kms. Therefore the \vmac\ of these stars were empirically adjusted for the code to work correctly. For some stars, the minimisation did not converge.

As a way of testing it, we computed values for the Sun (\teff=5777K, \logg=4.39, \feh=0.02) using the Vesta-reflected spectrum, for which we got \mbox{\vmac = 3.31 \kms} and \mbox{\vsini = 2.0$\pm$0.1\kms}. In \citet{doyle2014}, the \vsini\ adopted for the Sun was 1.9 \kms, which is in close agreement with the value computed in our study.

\subsection{Sulfur abundances}

\begin{figure*}
    \centering
    \includegraphics[width=0.95\hsize]{vesta_fits_two_sf.png}
    \includegraphics[width=0.95\hsize]{HD22879_fits_two_sf.png}
    \caption{Example of fitting profiles around \mbox{6743 \AA} (left) and \mbox{6757 \AA} (right). \textit{Top panels:} solar reflected spectrum from Vesta. \textit{Bottom panels:} spectrum of the metal-poor star HD22879 (\teff=5884K, \logg=4.45 dex, \feh $=-0.82$ dex, \vmac=3.46\kms , \vsini=1.37\kms). The synthetic profiles are for the best [S/Fe] value determined (before correction with respect to solar value) and for $\pm0.1$ dex deviation from it.}
    \label{fits}
\end{figure*}

\begin{table}
    \caption{Atomic parameters for the S lines used in this work (left to right): wavelength, excitation energy, oscillator strength, Van der Waals damping constant, literature reference for data. All lines belong to Multiplet 8.}
    \label{table:atomic:parameters}
    \centering
    \begin{tabular}{c c c c c}
        \hline\hline
        $\lambda$ & $\chi_{l}$ & \loggf & log($\gamma_{6}/\mathrm{N}_{H}$)  & Reference \\
        (\AA) & (eV)  & &  ($\mathrm{s}^{-1}\mathrm{cm}^3$) & \\
        \hline
        6743.4834  &   7.866  &  -1.27  &  -7.16 & \textit{emp.} \\
        6743.5400  &   7.866  &  -0.95  &  -7.16 &  \cite{kurucz2004}\\

        6743.6401  &   7.866  &  -0.93  &  -7.16 & \textit{emp.}\\
        6756.7500  &   7.870  &  -1.67  &  -7.16 & \cite{kurucz2004}\\

        6757.0000  &   7.870  &  -0.83  &  -7.16 & \cite{kurucz2004}\\
        6757.1750  &   7.870  &  -0.24  &  -7.16 & \cite{kurucz2004}\\
        \hline
    \end{tabular}
\end{table}
The determination of sulfur abundances was performed with the same package \textit{mpfit}, now setting [S/Fe] as the only free parameter. We fitted synthetic profiles obtained with MOOG to observational spectra of two \ion{S}{i} atomic lines from Multiplet 8\footnote{Numbering as in \citet{moore1945}.}, around \mbox{6743 \AA} and \mbox{6757 \AA}. Atomic parameters can be found in Table \ref{table:atomic:parameters}, and were obtained from \citet{kurucz2004, wiese1969}. The lines at wavelengths 6757.000 \AA\ and 6757.175 \AA\ were originally at 6756.960 \AA\ and 6757.150 \AA, respectively, and for the lines at 6743.483 \AA\ and 6743.640 \AA, the values of \loggf\ were slightly adapted. These changes were carried out so that the lines would better match the Kurucz Atlas solar spectrum and we could obtain A(S)$_{\odot}$=7.12 dex. A third S line around \mbox{6748 \AA} was considered, but inaccuracy in the line list ultimately prevented us from obtaining reliable abundances, and hence we discarded this line.

\citet{korotin2008, korotin2009} has studied departures from LTE and found the effects to be negligible on Mult. 8 (corrections are smaller than -0.1 dex). These lines are formed in denser layers of stellar atmospheres and are therefore less sensitive to non-LTE (NLTE) effects.

The $\chi^2$ analysis was performed separately in the intervals \mbox{6743.3-6743.8 \AA} and \mbox{6756.7-6757.4 \AA}, and the final [S/Fe] value is the mean of the two individual values, after being independently corrected with respect to the solar value.

Upon visual inspection of the fitting profiles, we decided to establish a cut-off temperature at \mbox{5000 K} because the spectra of cool stars were showing multiple lines that we could not reproduce due to incompleteness of the line list. Moreover, the used S lines have a high excitation potential and become very weak as the star becomes cooler. Unfortunately, these problems could not be solved and these stars had to be ruled out from the sample. We kept ten stars with temperatures below the cut-off \teff\ (although all with \teff$>$\mbox{4900 K}) whose synthetic profile was deemed to be accurate. Furthermore, we applied multiple S/N cut-offs for different \teff\ ranges to make sure our final results are as reliable as possible.

We tested our code by deriving the sulfur abundances of the Sun and found [S/Fe]$_{average}=\mathrm{-0.02}\pm\mathrm{0.02 dex}$. Figure \ref{fits} exemplifies the fitting of the synthetic profiles to observational data in both wavelength regions, for the solar spectrum and for the spectrum of the metal-poor star HD22879 (\feh $=-0.82$dex). After the fittings, all of the sulfur ratios derived for our sample were corrected with respect to the solar value obtained in the corresponding S line, and the average value was calculated afterwards.

\subsection{Uncertainties}

\begin{figure}
    \centering
    \includegraphics[width=0.95\hsize]{sfe_teff_feh_cor.png}
    \includegraphics[width=0.95\hsize]{sfe_logg_feh_cor.png}
    \caption{Relation of \sfe\ with \teff\ (top) and \logg\ (bottom), colour
    coded by metallicity. No obvious trends are detected.}
    \label{parameter:trends}
\end{figure}

\begin{table*}
    \caption{Sensitivity of the [S/Fe] ratio (in dex) due to errors on stellar parameter. The values presented are the means within each of the defined temperature subsamples.}
    \label{table:parameter:sensitivity}
    \centering
    \begin{tabular}{l c | l c | l c}
    \hline \hline
    Low \teff & $\Delta$\sfe & Solar \teff & $\Delta$\sfe & High \teff & $\Delta$\sfe \\
    \hline
    $\Delta$\teff$=\pm64$ K & $\pm0.03$ & $\Delta$\teff$=\pm24$ K & $\pm0.01$ & $\Delta$\teff$=\pm46$ K & $\pm0.02$ \\
    %
    $\Delta$\logg$=\pm0.17$ dex & $\pm0.05$ & $\Delta$\logg$=\pm0.03$ dex & $\pm0.01$ & $\Delta$\logg$=\pm0.05$ dex & $\pm0.01$ \\
    %
    $\Delta$\feh$=\pm0.04$ dex & $\pm0.02$ & $\Delta$\feh$=\pm0.02$ dex & $\pm0.02$ & $\Delta$\feh$=\pm0.03$ dex & $\pm0.03$ \\
    %
    $\Delta$\vmic$=\pm0.33$ \kms & $<0.01$ & $\Delta$\vmic$=\pm0.04$ \kms & $<0.01$ & $\Delta$\vmic$=\pm0.08$ \kms & $<0.01$ \\
    \hline
    \end{tabular}
\end{table*}
In this work, the errors in sulfur abundances are the quadratic sum of the line-to-line scatter and the effects that propagated from the errors in the stellar parameters. We note that some uncertainty may also arise from the automatic continuum placing, hence the importance of visually checking the fits and manually correcting, if necessary.

Table \ref{table:parameter:sensitivity} presents the mean errors of the parameters and the mean variation of sulfur when one of the stellar parameters is varied by their individual error. The sample was divided into three subgroups, as was done in A12 and DM17, to account for the dependence of all the parameters on the temperature of the stars, and so stars with \mbox{\teff $<$ 5277 K} are part of the "low \teff" subsample, stars with \mbox{\teff = $T_{\odot}\pm$500 K} belong to the "solar \teff" group, and lastly, "high \teff" includes the stars with \mbox{\teff $>$ 6277 K}.

As expected, the "low \teff" group is the most sensitive to errors in the parameters, whilst the "solar \teff" is the least. We can also see that the errors in microturbulence are practically negligible for the chosen lines.

\section{Results and discussion}

\begin{table*}
    \caption{Sample table of the derived \vmac, \vsini, sulfur abundance, error, number of S lines that were fitted, and signal-to-noise ratio of the spectrum.}
    \label{sample:table:parameters}
    \centering
    \begin{tabular}{l c c c c c c c c c}
    \hline \hline
    Star & \teff\ & \logg\ & \feh\ & \vmac\ & \vsini\ & \sfe\ & $\sigma_{\mathrm{[S/Fe]}}$ & \textit{n}$_{\mathrm{[S/Fe]}}$ & S/N \\
    \hline
    ...   &   ...   &   ...  &  ...  &  ...  &  ...  &  ...  & ...  &  ... & ... \\
    HD127124   &   5030.0   &   4.55  &  -0.03  &  2.37  &  0.51  &  -0.03  &  0.10  &  2 & 218 \\
    HD13808    &   5033.0   &   4.51  &  -0.21  &  2.44  &  0.50  &   0.08  &  0.17  &  2 & 1015 \\
    HD191797   &   5037.0   &   4.62  &  -0.09  &  2.22  &  4.10  &  -0.07  &  0.15  &  2 & 321 \\
    HD17970    &   5038.0   &   4.54  &  -0.45  &  2.38  &  0.27  &   0.20  &  0.13  &  2 & 338 \\
    ... & ... & ... & ... & ... & ... & ... & ... & ... & ... \\
    \hline
    \end{tabular}
\end{table*}

We successfully derived [S/Fe] ratios for 719 stars from our sample. For 706 of them, the sulfur abundance presented is the mean of the values obtained from the two lines, whereas for the other 13 stars, the abundances could only be derived from one of the lines. Figure \ref{parameter:trends} presents the relationship between \sfe\ and \teff\ and \logg. It is clear that there are no systematic trends of the abundance ratios caused by the \teff\ or \logg\ parameters, but the colour scheme shows a trend of increasing \sfe\ with decreasing \feh. This trend is expected from the GCE, as metal-poor stars usually have higher \sfe\ ratios. Table \ref{sample:table:parameters} shows a sample of our results as well as some of the stellar parameters derived in previous works.

Below, we analyse our results in some different contexts.

\subsection{[S/Fe] vs. [Fe/H]}
\begin{figure}
    \centering
    \includegraphics[width=0.95\hsize]{sfe_feh_error_bars_cor.png}
    \caption{\textit{Top:} \sfe\ vs \feh\ with error bars. The stars with largest errors are usually those that had abundance derived from one line only.}
    \label{sfe_feh}
\end{figure}

\begin{figure}
    \centering
    \includegraphics[width=\hsize]{comparison_2.png}
    \caption{Comparison of [S/Fe] ratios with values found in the literature. Average deviation of all points is displayed in the bottom right. References: a) \cite{maldonado2016}; b) \cite{takeda2016}; c) \cite{mishenina2016}; d) \cite{duffau2017}; e) \cite{caffau2019}.}
    \label{comparison}
\end{figure}

In Fig. \ref{sfe_feh}, we depict the sulfur abundances ratios against metallicity. The plot includes the total error bars associated with the derivations. The stars with the largest errors are mostly stars that had abundances derived from only one line.

From our results, the abundances of sulfur appear to be decreasing towards higher metallicities, with \sfe\ values tending to $\sim-0.1$ at \feh\ $\sim0.25$. From solar metallicities down to \feh\ $\sim-0.25$, the \sfe\ ratios are close to solar, and with further decreasing metallicity, an increasing trend is very clearly distinguished. At around \feh\ $=-0.75$, despite some scatter, the ratios appear to stabilise and form a plateau at \sfe\ $\sim0.3$. This behaviour is very typical of $\alpha$-elements, and thus has been the theoretical expectation for sulfur.

To help ascertain which of the different trends that have been proposed with respect to the GCE of sulfur is more accurate, we would have to analyse stars below the \mbox{\feh\ $=-1.0$ dex} threshold. Unfortunately, despite the initial sample containing stars with metallicities as low as $-1.39$ dex, the sample for which we could derive \sfe\ ratios only includes two stars with \mbox{\feh\ $\leqslant-1.0$}. This is due to the fact that the lines from Mult. 8 used in this work are difficult to detect in metal-poor stars. Nonetheless, if we look closely at these two metal-poor stars, both of them have \sfe\ values around 0.35, which lends some support to the existence of a flat trend at the metal-poor regime.

In general, our results of \sfe\ vs \feh\ are in good agreement with those of recent studies by \citet[taking into account that NLTE corrections were not applied in this work]{mishenina2015, takeda2016, duffau2017, caffau2019}.

Furthermore, we searched the literature for stars in common with the ones from our sample so as to compare the derived \sfe\ ratios to the ones derived in other works. The comparison of our \sfe\ ratios to those of \cite{maldonado2016, takeda2016, mishenina2016, duffau2017, caffau2019} is plotted in Fig. \ref{comparison}. The samples used by these authors had 12, 19, 8, 4 and 5 stars in common with our own sample, respectively, which yielded an average deviation ($\sigma_{av}$) for each of the comparison works of 0.07, -0.03, -0.05, -0.09 and 0.09 dex, respectively. The values derived in the comparison works are in good agreement with our abundance ratios. Appendix A contains the full table of \sfe\ ratios for each star in common with the aforementioned literature.

\subsection{Galactic populations and [S/Fe]-age relation}

\begin{figure}
    \centering
    \includegraphics[width=0.95\hsize]{alpha_delgado_mena+17_updated_line.png}
    \includegraphics[width=0.95\hsize]{sfe_fe_populations_5277_6277K_updated_line.png}
    \includegraphics[width=0.92\hsize]{sfe_fe_populations_average_5277_6277K.png}
    \caption{\textit{Top:} \alphafe\ vs \feh, data from DM17. The black line is the updated $\alpha$ separation line, also from DM17. (see text for more detail). \textit{Middle:} [S/Fe] vs [Fe/H], with the same $\alpha$-line as the top panel. \textit{Bottom:} Average [S/Fe] for each metallicity bin (of width 0.1 dex) per population. The numbers indicate the size of the sample of each population in each bin. \textit{Symbols:} yellow circles are for the thin disk, blue triangles for the thick disk, red squares for the high-$\alpha$ metal-rich stars, and purple diamonds for halo stars.
    }
    \label{sfe:feh:pops}
\end{figure}

\begin{figure}
    \centering
    \includegraphics[width=0.95\hsize]{alpha_sep_hist_cor_paint.png}
    \caption{[Fe/H] and [S/Fe] separation histograms for stars of the thick disk and \hamr\ (high-$\alpha$ sequence). The vertical lines indicate the low-density regions found in \cite{adibekyan2011}, at \mbox{\feh\ $=-0.2$} dex (top histogram) and \mbox{\alphafe\ $\sim0.17$} dex (in the lower histogram, we plot the line at the same value of sulfur abundance: \mbox{\sfe\ $=0.17$} dex).}
    \label{sfe:histograms}
\end{figure}

\begin{figure}
    \centering
    \includegraphics[width=0.95\hsize]{sfe_age_small_err_populations_cor.png}
    \includegraphics[width=0.95\hsize]{sulfur_feh_age.png}
    \caption{\textit{Top:} [S/Fe] vs age, symbols for galactic populations as in Fig \ref{sfe:feh:pops}. \textit{Bottom:} Distribution of stellar age in the \sfe\ vs \feh\ plane. The sample depicted in both panels is composed only of stars with age uncertainties lower than 1.5 Gyr.
    }
    \label{sfe:age:pops}
\end{figure}

The Milky Way's thick disk was discovered over three decades ago by \cite{gilmorereid1983}. To the present day, it is still not clear which is the best method to accurately separate stars of the thin and thick disk \citep[e.g. kinematically, chemically, via age, see][and references within]{buder2018}, or even whether more populations (or sub-populations) should be considered \citep{adibekyan2011, chiappini2015, martig2015, rojas-arriagada2016}.

The stars in our sample were classified as described in \citet{adibekyan2011, adibekyan2013}, according to the chemical separation observed in [$\alpha$/Fe] ($\alpha$ being the average of Mg, Si, and Ti) across different metallicity bins, using the updated abundance ratios derived in DM17. The line that separates the low- and high-$\alpha$ sequences in the \alphafe\ vs \feh\ plane was first presented in \cite{adibekyan2011} and later updated in DM17 (see their Fig. 9). The updated line is shown in Fig. \ref{sfe:feh:pops} and will henceforth be referred to as the $\alpha$-line.
Exceptionally, halo stars were categorised on the basis of kinematics. We will refrain from commenting on the abundances of the halo stars as they are only three.

Our sample is composed of 600 thin disk stars, 74 thick disk stars, 42 from the \hamr\ group (explained in the following paragraph), and 3 from the Galactic halo. The different stellar populations are plotted in the middle panel of Fig. \ref{sfe:feh:pops} in the \sfe\ vs \feh\ plane.

Adding to the well-known thin and thick disk populations, the works of \citet{adibekyan2011, adibekyan2013} revealed a potential new group of Galactic disk stars with high metallicity (\mbox{\feh\ $>-0.2$} dex) and enhanced [$\alpha$/Fe] ratios compared to the thin disk, hence called the high-$\alpha$ metal-rich (hereafter \hamr) stars. The \hamr\ and the thick disk populations form the \mbox{high-$\alpha$} sequence, and the separation between the two comes from the analysis of histograms depicting the stellar distributions in [Fe/H] and [$\alpha$/Fe], where well-defined minima (low-density regions) were found (see Fig. \ref{sfe:feh:pops}). More recently, other authors have investigated a possible separation between these two populations, but most often found a continuous distribution rather than clear separations, suggesting that \hamr\ stars were simply the metal-rich tail of the thick disk \citep{recioblanco2014, bensby2014, buder2018}, enriched by both SNe II and SNe Ia. In this paper, we will investigate how the abundances of sulfur fit into the proposed populations.

In the upper panel of Fig. \ref{sfe:feh:pops}, we display the \alphafe\ ratios (where $\alpha$ includes Mg, Si, TiI, and TiII), derived in DM17, against metallicity, for comparison with the \sfe\ ratios from this work, which are depicted in the middle panel, also against metallicity. In both panels, we include only stars with \mbox{\teff = $T_{\odot}\pm$500 K} and we over-plotted the aforementioned $\alpha$-line. The data from DM17 and our own data show similar distributions for each of the populations, although our \sfe\ ratios are more scattered and the populations are less well separated. The $\alpha$-line does not accurately separate the two low- and high-$\alpha$ sequences in the \sfe\ vs \feh\ plane, but it should come as no surprise that not all $\alpha$-elements behave exactly in the same way. In this case, we know sulfur typically has large errors, hence there is a greater deviation and the separation may have become blended as a result.

The bottom panel of the same figure shows the average \sfe\ ratio in each metallicity bin, for each population. As expected, the populations of thick and thin disks clearly follow different $\alpha$-enrichment trends, with thick disk stars dominating the low-metallicity regime with higher \sfe\ ratios, whereas conversely, the thin disk stars are metal-richer but poorer in sulfur. In this panel, we can see that \hamr\ stars do display noticeably higher \sfe\ ratios than the thin disk counterparts at the same metallicity.

With regard to the separation between thick disk and the \hamr\ group, Fig. \ref{sfe:histograms} shows histograms of the same type as those analysed in \cite{adibekyan2011}, which reported low-density regions at \mbox{\feh\ $=-0.2$ dex} and \mbox{\alphafe\ $\sim0.17$ dex}. Although for metallicity, there is an unmistakable minimum around \mbox{\feh\ $=-0.2$ dex}, the same cannot be said for the \sfe\ distribution. The separation would be expected at a \sfe\ ratio close to 0.17 dex, and despite the presence of a smaller number of stars in this bin (compared to the adjacent ones), the remaining distribution is too irregular and does not allow for a confirmation of this separation.

We performed two-sample Kolmogorov-Smirnov tests on the \sfe\ ratios of the different population samples (thin/thick, thin/\hamr, thick/\hamr) and all of them yielded p-values of magnitude $10^{-8}$ or smaller, rejecting the hypothesis that the stars were drawn from the same population.

We also obtained stellar ages for our sample from \citet{dmena2019}, which the authors derived using the PARAM v1.3 tool with Parsec isochrones \citep{bressan2012} and \textit{Gaia} DR2 parallaxes (we refer the reader to these papers for more information on the derivation process and for an analysis of abundance-age ratios of various elements). The relationship of \sfe\ ratios and age is shown in the upper panel of Fig. \ref{sfe:age:pops} and the lower panel depicts the \sfe\ vs \feh\ plane with colour according to stellar age. Both panels include only stars with an error in age lower than 1.5 Gyr. The trend of \sfe-age is very similar to other $\alpha$-elements, with a linear increase with age for the thin disk stars and a more exponential increase for the old thick disk stars \citep[see for comparison Fig. 5 in][]{dmena2019}. The \hamr\ stars present intermediate ages between both populations and follow the increase with age of thin disk stars. The thin disk population can be fitted by a slope of $0.011\pm0.001$, which is similar to those given in \citet{dmena2019} for the $\alpha$-elements Mg, Si, Ca, TiI, and TiII.

\subsection{Theoretical predictions for [S/Fe]}

\begin{figure}
    \centering
    \includegraphics[width=0.95\hsize]{kobayashi_two_models.png}
    \includegraphics[width=0.95\hsize]{romano2010_cor.png}
    \includegraphics[width=0.95\hsize]{prantzos2018_cor.png}
    \caption{Comparison of observational data to theoretical models. \textit{Top panel:} Models from \citet{kobayashi2006, kobayashi2011}; \textit{Middle panel:} Models 1, 4, and 5 (as numbered in paper) from \citet{romano2010}; \textit{Bottom panel:} Model from \citet{prantzos2018}}
    \label{models}
\end{figure}

We compare the \sfe\ ratios obtained in this work to model predictions from different authors \citep{kobayashi2006, kobayashi2011, romano2010, prantzos2018} in Fig. \ref{models}. There is a clear distinction in the shape of the lines that represent the evolution of sulfur predicted by the different models.

The top plot of Fig. \ref{models} shows the models of \citet[hereafter K06]{kobayashi2006} and \citet[hereafter K11]{kobayashi2011}. Both these models consider the yields by SNe and hypernovae (HNe) explosions, but whereas K06 defines the HNe fraction as 0.5 regardless of mass or metallicity of the star, K11 defines a fraction of 0.5 only for stars with mass greater than 20 M$_{\odot}$. K11 also includes yields of asymptotic giant branch (AGB) stars. These two models are the ones that best describe the overall chemical evolution of sulfur. They trace the lower \sfe\ ratios of the thin disk and then raise towards lower metallicities to accompany the thick disk abundances, showing a "knee" feature at \feh\ $\sim-1$, where they go on to form a  plateau. These models are the best fit for the thick disk stars as they accurately fit the \sfe\ ratios at low-metallicity, especially the model from K11.

The middle plot presents three models from \citet{romano2010}. Model 1 (models are numbered as in the paper) adopts the yields of \citet{woosleyweaver1995} case B, while models 4 and 5 adopt the yields of K06, with HNe fractions for massive stars of 1 and 0, respectively. These models underestimate the abundance ratios throughout the entire metallicity range, inaccurately representing the evolution of sulfur. Model 4, however, does present higher \sfe\ values in the very metal-poor regime, which is most likely a product of the high HNe fraction.

Lastly, in the bottom plot, the model from \citet{prantzos2018} is depicted, which adopts the yields of \citet{cristallo2015a} for low and intermediate mass stars and those of \citet{limongichieffi2018} for massive stars, which include mass loss and rotation. This model describes well the \sfe\ ratios of the thin disk, but underestimates the thick disk abundances. A more pronounced slope starting at \feh\ $\leqslant-0.5$ would be expected, following the rise of abundance ratios. This may be due to the fact that no high-energy supernovae explosions (or HNe) were included in the model.

From comparison with our results, the best explanation for the \sfe\ evolution of our sample is a combination of yields from SNe and HNe at high stellar masses and AGB (models by K11).

\subsection{Planet hosts vs. non-planet hosts}

\begin{figure}
    \centering
    \includegraphics[width=0.95\hsize]{sfe_feh_planet_hosts_in_population_cor.png}
    \includegraphics[width=0.95\hsize]{average_sfe_planets_nrs_cor.png}
    \caption{\textit{Top:} Planet hosts vs non-planet hosts, with different colours for planet mass and different symbols for population, as indicated in the legend.
    \textit{Bottom:} Averages of [S/Fe] in each metallicity bin for stars without planets (black circles), jovian-mass hosts (red downwards triangles), and neptunes/super-Earth hosts (blue pentagons).
    }
    \label{sfe:planets}
\end{figure}

\begin{figure}
    \centering
    \includegraphics[width=0.98\hsize]{planets_histograms_cor.png}
    \caption{Percentage of stars with giant/neptunian planets within the planet host sample against metallicity (left) and [S/Fe] (right).}
    \label{hist:feh:planets}
\end{figure}

Our sample of stars with derived sulfur abundances contains 134 stars with known planetary companions, with 110 of them hosting jovian-mass planets while the remaining 24 host Neptune-like planets or Super-Earths. In the top panel of Fig. \ref{sfe:planets}, we can see the distribution of stars with exoplanets (coloured in blue and red) and the comparison sample (empty shapes). The lower panel of Fig. \ref{sfe:planets} displays the average \sfe\ ratios of each of the subsamples (non-planet hosts, giant planet host, and Neptune/Super-Earth planet host) in each metallicity bin.

The behaviour of the planet hosts (PH) and non-planet hosts (NPH) seems rather similar, not showing any distinctive trends or differences. The \sfe\ ratio averages do not reveal any specific trends of under or overabundance with respect to each other, but rather an irregular distribution for \mbox{\feh$>-0.3$}.

We note that for \mbox{\feh$<-0.3$}, our average ratios of both types of PH suffer from small-number statistics, and having one single planet host star per bin can, in no way, be taken as representative of the reality. We may be tempted to point out that PH seem to have higher sulfur abundances at lower metallicities, and in fact, with higher number statistics, it has been found that other $\alpha$-elements are indeed enhanced in metal-poor PH (Mg, Si, and Ti, see A12). However, in this work, we need to keep in mind the extremely reduced sample size for this metallicity range.

Many studies of PH vs NPH show trends of over or under-abundances for other elements, but it is important to note that many of these were based on small samples or rely on comparison samples of 'single' stars that had not been searched for planets, hence not knowing if the stars hosted at least massive planets. Our sample is large enough to allow us to take meaningful conclusions, at least for the range \mbox{\feh$>-0.3$}, regarding the differences (or lack thereof) when comparing sulfur abundances of stars with and without known planetary companions.

\cite{ecuvillon2004a, ecuvillon2004b} studied volatile elements N, C, S, and Zn in a sample with a metallicity range of $-0.8\leq$ \feh\ $\leq 0.5$ dex and reported no differences in any of these ratios. On the other hand, in \cite{dmena2018}, [Zn/Fe] was found to be overabundant in planet hosts at low metallicity, which is probably driven by the fact that Zn follows the same evolution as $\alpha$-elements, despite not being such an important element for planet-formation as Mg or Si.

Regarding the likelihood of planet formation around certain types of stars, it has been well established that giant planetary companions are much more likely to orbit metal-rich stars, whereas lower mass planets tend to orbit stars of slightly lower metallicity \citep[e.g.][]{sousa2011, buchhave2012}. This tendency can be confirmed in the left-hand plot of Fig. \ref{hist:feh:planets} (only including stars for which we could derive sulfur abundances). On the right-hand plot of the same figure, we find the distribution of planet hosts according to the stars' \sfe\ ratio. The most evident characteristic is that both giant and Neptune/Super-Earth-sized planets seem to form more often around solar-abundance stars ($-0.1<$\sfe$<0.1$). Additionally, we find that lower mass planets are more likely to orbit stars with higher sulfur ratios (thick disk) rather than lower (thin disk).

\section{Summary}

We performed spectral synthesis on a sample of 1059 \mbox{HARPS-GTO} solar neighbourhood stars, for lines of Multiplet 8 (triplets at \mbox{6743 $\AA$} and \mbox{6757 $\AA$}), having obtained \sfe\ ratios for 719 of the stars and for the Sun, through a Vesta-reflected spectrum. A third triplet at \mbox{6748 $\AA$} was considered, but discarded due to incorrect fitting of the models. Values of rotational velocity were also determined for most stars of the initial sample.

The results were interpreted in the context of the \sfe\ vs \feh\ plane, the distribution of sulfur in Galactic populations, how sulfur abundances relate to stellar age, the evolution of sulfur according to theoretical models of Galactic chemical evolution and, finally, comparing abundances of planet-hosts and non-planet hosts. Our conclusions can be summarised as follows:

\begin{enumerate}
    \item In the \sfe\ vs \feh\ plane, sulfur appears to behave like a typical $\alpha$-element, showing the expected trend  with solar-abundances around solar metallicity and a rise towards lower metallicities. There is an apparent decrease of the \sfe\ ratios towards higher metallicities, although this should be taken with caution due to having few stars at this extreme. Similarly, we can not confidently state that the ratios form a plateau for \mbox{\feh$<-1.0$ dex} due to the small number of stars below this threshold.
    \item The distribution of sulfur ratios in the Galactic populations is also $\alpha$-like. The thin and thick disks overlap slightly in the chemical plane but are clearly separated overall. Sulfur-enhanced and older stars are identified as belonging to the thick disk population whereas younger stars are sulfur-poor and categorised as thin disk members.
    \item The $\alpha$ separation line \citep[presented in][and updated in DM17]{adibekyan2011} was not able to visually separate the low- and high-$\alpha$ sequence in a very accurate manner, but this can be due to large uncertainties in sulfur abundances and differences in the nucleosynthesis of this element compared to those of other $\alpha$-elements. Nevertheless, it has been confirmed that the high-$\alpha$ metal-rich stars are, on average, sulfur-enhanced compared to the thin disk counterparts of the same metallicity, similarly to their enhancement of other $\alpha$-elements. Statistically, the Kolmogorov-Smirnov tests performed on the \sfe\ ratios of the thin disk, thick disk, and \hamr\ group reject the hypothesis that the stars were drawn from the same population.
    \item The \sfe-age relation is very clear and similar to those found for other $\alpha$-elements in \cite{dmena2019}, reinforcing that $\alpha$-abundances are a good proxy for stellar age.
    \item In the metal-poor regime, the \sfe\ vs \feh\ distribution is best fitted by the models of \cite{kobayashi2006, kobayashi2011}, as they follow the rise of the [S/Fe] ratios towards lower metallicities, placing the 'knee' of the thick disk evolution at around \feh$=-1.0$. These models included normal energy and high energy supernovae explosions, although in different fractions, and \citet{kobayashi2011} also included AGB yields. As for the metal-rich tail, the evolution of the sulfur ratios are best described by the model of \cite{prantzos2018}, who considered only "typical" energy supernovae. Nonetheless, we note that none of the models reach the high metallicities presented in this work.
    \item We find no evidence of under or overabundance of \sfe\ when comparing the average ratios of stars with and without planetary companions. This lack of differences between the two groups of stars was also reported in \cite{ecuvillon2004a, ecuvillon2004b} for other volatile elements. For metallicities below -0.3 dex, firm conclusions regarding the abundance comparisons cannot be reached due to the small number of planet host stars in these metallicity bins. Even so, for the few metal-poor planet hosts for which we could derive \sfe\ ratios, it is enhanced, despite the difference with respect to thick disk stars without planetary companions not being relevant.
    \item Planet companions are more common around stars with solar-abundances of sulfur, regardless of the planet mass. Lower mass planets seem more likely to orbit sulfur-enhanced stars rather than sulfur-depleted, although still with much lower frequency than around solar-abundance stars.

\end{enumerate}

All in all, sulfur can be considered as a typical $\alpha$-element for all purposes of Galactic chemical evolution, Galactic populations and ages. With regard to planet host stars, abundances of this volatile element are no more abundant or scarce than in those without planetary companions. There is a necessity for future studies covering the low-metallicity range, which will help clarify some details which could not be analysed in our data, as well as place further constrains in important formation mechanisms of our Universe. Moreover, it would be interesting to have models of \sfe\ evolution for \feh\ $\geqslant 0.25$ dex, since our data seem to point to a continued decrease at high metallicities, but the models which best fit our sample in this region \citep{prantzos2018} present a rather flattened trend with increasing metallicity.

\begin{acknowledgements}
     We thank Alejandra Recio-Blanco and Patrick de Laverny for fruitful discussion, Vardan Adibekyan for useful suggestions, and the anonymous referee for helpful comments which helped improve this paper. A.R.C.S., E.D.M. and M.T. acknowledge the support by FCT/MCTES through national funds (PIDDAC) by this grant UID/FIS/04434/2019. This work was also supported by FCT - Fundação para a Ciência e a Tecnologia through national funds (PTDC/FIS-AST/7073/2014) and by FEDER - Fundo Europeu de Desenvolvimento Regional through COMPETE2020 - Programa Operacional Competitividade e Internacionalização (POCI--01--0145-FEDER--016880). A.R.C.S. acknowledges the support by the Student Initiation Fellowship funded by the grant UID/FIS/04434/2013 \& POCI--01--0145-FEDER--007672. E.D.M. acknowledges the support by the Investigador FCT contract IF/00849/2015/CP1273/CT0003 and in the form of an exploratory project with the same reference.
\end{acknowledgements}

\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


text:
Index of Locations
Entries by County
Name Dropping
Age Is No Handicap
Photos from May, 2008.
Normally when I research a factory it becomes clear pretty quickly what the primary address of the facility was, and it usually points to the plant's front office building—in the case of the Detroit Insulated Wire Co., neither was true. Almost every mention of the company in books or newspapers referenced the intersection of Wesson and Albert (Nowak) Streets rather than an address. It took a long time to figure out, but the only real address I ever saw the place referred to by was 4647 Wesson, which was not the front office, but one of the warehouses on the corner.
In 1906 under the supervision of Reuben Sloan, superintendent of the Solvay Process Works, the first buildings of this factory were built on the site of "the old west side brick yard," with the bottom of the old clay pits "forming a solid foundation" according to an article in the Detroit Free Press. I'm not sure why Solvay was involved in this, but that's what the article said.
The c.1897 Sanborn map shows this block as empty land, and by the c.1910 map, only one building was erected, right on the railroad spur. A city atlas from 1885 corroborated this being the site of an old brick yard.
The three-story office building (seen at left, above) was built in 1920, while the big four-story concrete structure wasn't even built yet on the c.1924 map. Most of the complex was made up of single-story buildings with shed or "sawtooth" type roofs.
Detroit Insulated Wire Co. was organized and incorporated in 1906 by ex-Pittsburghers who came to the conclusion that Detroit was the ideal place to put a copper wire factory due to its proximity to the copper supply chain, rail and waterway shipping, and a ready labor market. They started small, just making wire for "code and telephone" cables (I assume "code" means telegraph use). They eventually expanded production to include wire gauge sizes from as fine as a strand of silk to as large as two inches in diameter, most of it insulated with rubber coating. Many of their products were used in the automotive industry as well, and they were covered in cambric varnished tape and saturated varnished braids. They also produced "armored" wire cable, which I presume to be the old-timey equivalent of today's "Greenfield," which is a flexible metal conduit.
The article said that Detroit Insulated Wire Co.'s products could be identified by the presence of three uncolored threads laid parallel between the rubber insulation and the braid. This company was the only one of its kind in Michigan, and only one of three west of the Alleghenies. It had nonetheless become the largest exclusive manufacturer of rubber insulated cables in North America, with an output of a million feet of wire per day.
Detroit's position directly along the export route of pretty much all raw industrial production copper in the world made it a natural place for a wire-making firm. So it's a wonder this was the only one, seeing as every other manner of malleable metalworking firm has existed here since copper was first being mined in Upper Michigan by white settlers in the 1840s.
The company president of Detroit Insulated Wire was Joseph H. Hunter, who began his career with the Allegheny County Light Co., managed the Pittsburgh Light Co., and later became general manager of the National Cable & Wire Co. He was also manager of the Ferrous Chemical Co. of Pittsburgh, where he was associated with Professor Julius A. Koch. The company superintendent of Detroit Insulated Wire was John S. Lucock (of National Cable & Wire Co.), its secretary Charles C. Gray (of National Cable & Wire Co. and Westinghouse, Pittsburgh & Allegheny Telephone Co.), and its treasurer was William G. Dalgleish.
Detroit historian Clarence M. Burton wrote that Mr. Hunter was hailed as a leader amongst the men of industry called to Washington D.C. in WWI to help aid the war effort, for his idea in distinguishing different branches of the Signal Service on the French front. Hunter held a few patents for electrical appliances, and also had a keen interest in photography.
In 1913 the plant's floor space was 60,000 sq.-feet, and their products were known "from Canada to the Panama Canal" according to the Michigan Manufacturer & Financial Record that year. They also had bowling and baseball factory teams. In the 1920s the plant employed around 350 people.
Having been a one-time electrician myself, and having spent plenty of hands-on time working with vintage wiring from this time period while restoring my c.1887 house, I'm familiar with this type of insulated wire. It's amazing to me that this stuff is still around in houses that are still lived in, and it is still being used for electricity, over 100 years later. Left alone, it can function admirably for a very long time, but as we handymen know, rarely is anything in a house that old left alone.
Usually when you find this stuff in a house now, it dies when you touch it. The "rubber" insulation crumbles like hard clay, and the ends of the copper conductor have become so fatigued with being spliced and re-spliced over the decades that it is unworkable and prone to breaking. To say nothing of its other inadequacies and dangers. That said, when I bought my c.1887 house, that is the type of wire that was in active use for electrical service...I painstakingly replaced all of the "knob & tube" circuits with new wiring that I *hope* will last as long.
Thanks to the magic of Google Books, I was able to learn something more about Detroit Insulated Wire. The 1973 Senate hearings on the Industrial Reorganization Act regarding the Communications Industry in revealed that prior to 1930, the Bell System met all of its insulated wire and cable needs from seven different suppliers to Western Electric, of which Detroit Insulated Wire Co. was one (the other cable suppliers were all based in New York, Massachusetts, or Connecticut). So in other words this ragged factory most likely helped supply the grand construction program that facilitated the linking of the United States by telephone at the dawn of the Technology Century. It produced telephone cables not only for Detroit, but most likely for greater Michigan and the Midwest.
After 1930 however, all of the Bell System's wire and cable was manufactured by Western Electric, and all other supply contracts were cancelled. As a result, all of the former wire suppliers were out of business by 1935, except Whitney-Blake and General Cable Co. Mr. Hunter sold the Detroit Insulated Wire Co. in 1932, to General Cable Co. of New York. Production of wire most likely ceased at that time, because the next occupant of this facility seems to have been the Great Lakes Thread & Yarn Co., judging from a help wanted ad from May 1934.
That company remained here until at least 1944. Other help wanted ads during WWII called for men with machine-operating experience for war work, declaring, "Age is no handicap." Great Lakes Thread participated in war production, and also participated heavily in the drives for war bonds. I don't know what exactly the company may have produced for the war effort, perhaps things such as military uniforms, vehicle seats, backpacks, or tents?
Later news blurbs in 1955 and 1961 seemed to imply that the Cadillac Motor Division had been using the plant, so possibly the facility was split between them and Great Lakes Thread? Cadillac said in 1961 that it would discontinue manufacturing of army tank transmission parts at this plant by mid-June. Due to the low volume, the work would be taken over by GM's Allison Division, for which Cadillac produced the parts. Sixty-five men worked here under Cadillac, and the future of the plant itself was not decided yet at the time of the article.
Cavemonkey, a colleague of mine from Colorado who is also a WWII buff tells me that if Cadillac was using this plant for manufacturing tank transmission parts, it would have been for the M5 Stuart and later the M24 Chaffee tanks. As a matter of fact, Cavemonkey was with me the day I explored this factory. Cadillac also produced Allison aircraft engines in Detroit, so that could have been done here as well, he said.
Meanwhile, another entity had moved in as well, as evidenced by a help wanted ad for a printing press operator in 1955. I believe that this is when the Catholic Archdiocese of Detroit came to own at least part of the factory. The Bible Press Company was listed here from about 1955 to at least 1962, and the Church and School Equipment Co. was listed here from at least 1961 to 1965, both of which were in some way affiliated with the Archdiocese, which owned the property. Ads in newspapers offered products from these companies, including tubular steel folding chairs, tape recorders, and "Cathedral Hi-Fi Tape," as well as a "catalogue of over 900 Redi-Recorded tapes."
From then until the 1970s I was only able to come up with one other tenant for this building, from a help-wanted ad for a machine repairman that was posted in the May 1970 Free Press, indicating it was then occupied by the Detroit Parts Warehouse, Inc., which seems to have stocked automotive parts.
It looks like the firemen employed heavy equipment to bash holes in the walls to get water on the blaze. The church seen above is St. Francis d'Assisi, a once large Catholic parish for this once densely Polish neighborhood. It was built in 1903, making it three years older than the plant. I have been inside the church, maybe one day I will post my pictures.
You may recall that I also explored the abandoned firehouse of Detroit Fire Department Engine 22 nearby, in an older post.
This factory complex met its doom on October 16, 2005, in one of the worst fires in Detroit's recent history. These days the Detroit Fire Department rarely calls out five alarms, even for fires that other cities would consider cataclysmic, but this one merited all five bells (you may recall that the old Studebaker Plant #5 was also destroyed that same year by a five alarm blaze). Had the old Engine 22 firehouse—which is less than two blocks away—not been abandoned, it is likely that this factory may have had a different fate.
This entire complex was annihilated by burning plastics and other troublesome fuels...the thing about plastics fires is that they really don't want to be extinguished once they start burning. And with Detroit's notorious issues with non-working hydrants and low pressure, it's a miracle the fire was put out at all. I remember the day it burned...I happened to be driving on Warren Road, over 20 miles to the west, and I still saw the towering column of black smoke rising from this disaster scene as if it were just a few blocks away.
I did not explore the upper levels of this factory; after viewing the completely crumbled condition of these support columns, I decided that there couldn't be much on the other floors that was worth my life to see. Of course, the building proved to still be much sturdier than I calculated...I thought the place would collapse if I farted too loud, but even in this condition it remained standing another decade. Reinforced concrete is incredibly hard to defeat.
The building was still owned at the time of the fire by a Bloomfield Hills-based company called Intermet, which had been cited often by state officials on storage of tires and other waste, going back to 1993. Intermet paid no fines at the time because the violations were corrected, according to the Free Press. Intermet owner Julius Rim expressed remorse to reporters that the fire had occurred, which sent noxious smoke into surrounding neighborhoods and cost the taxpayers plenty of money to extinguish. Intermet was an automotive supplier for Ford, Delphi, and Daimler-Chrysler, making brake and suspension parts, and they had just filed for Chapter 11 bankruptcy exactly one year prior to the fire.
Fire officials stated that the fire was fueled by propane tanks in the buildings, as well as mystery drums of unknown liquids, and old junk cars. The fire started in a single-story warehouse-turned-junkyard, and then quickly spread to a plastics company in the taller building.
Yes, that brick is f@#$%ing melted. Brick. Melted.
The remaining ruins of the plant were torn down by 2017.
Sanborn Maps of Detroit, Vol. 12, Sheet 49 (1924)
Sanborn Maps of Detroit, Vol. 5, Sheet 9 (1910)
E. Robinson Atlas of the City of Detroit and Suburbs (1885)
"Employment for 1,500 Men," Detroit Free Press, November 12, 1906, p. 9
"Adds Sprinkler System," Detroit Free Press, March 13, 1913, p. 16
Michigan Manufacturer & Financial Record, Vol. 13, No. 16 (April 1913), p. 49-51
The City of Detroit, Michigan, 1701-1922, Volume 4, by Clarence Monroe Burton, William Stocking, Gordon K. Miller, p. 58-60
The Book of Detroiters (1908), by Albert Nelson Marquis, p. 213-214, & 243
The Industrial Reorganization Act: Hearings Before the Subcommittee on Antitrust and Monopoly of the Committee on the Judiciary, United States Senate, 93rd Congress, First Session on s.1167, Part 2: The Communications Industry, (July 30-August 2, 1973) p. 628
"J.H. Hunter, Industrialist, Dies at 84," Detroit Free Press, August 26, 1952, p. 2
Help Wanted ad, Detroit Free Press, May 13, 1934, p. 1
"This Message Sponsored by These Public Spirited Firms," Detroit Free Press, November 15, 1942, p. 10B
"War Bonds To Have and to Hold," Detroit Free Press, May 14, 1944, p. 4-8
Detroit Free Press, January 9, 1955, p. 40
Advertisement, Detroit Free Press Roto, April 13 1958, p. 8
"Cadillac Drops Tank Parts Work," Detroit Free Press, May 24, 1961, p. 35
"Churches Pay Full Taxes On Outside Properties," Detroit Free Press, Mar 20, 1962, p. 3
Advertisement, Detroit Free Press, March 13, 1964, p. 10B
Advertisement, Detroit Free Press, December 19, 1965
Help Wanted ad, Detroit Free Press, May 23, 1970, p. 6B
"Officials See No Concern Around Detroit Tire Fire," Detroit Free Press, October 18, 2005, p. 3B
"Auto Supplier Intermet Files For Bankruptcy Aid," Detroit Free Press, October 1, 2004, p. 1C
"Big Blaze Is Seen For Miles," Detroit Free Press, October 17, 2005, p. 3B
Labels: Detroit Insulated Wire Co., Wayne County
Photos from June, 2013.
I don't always set out to get into places I don't belong, but sometimes it just happens. This was one of those times.
Every year I go to the Irish Festival at St. Patrick's Catholic Church, which is near Orchestra Hall in Detroit. My exploring partner Sloop has family who have been involved in the parish for many years.
The story of St. Pat's is a little confusing...the original St. Patrick's Church was in the Brush Park neighborhood, at 124 Adelaide. The parish was begun in 1862 as Irish moved northward from Corktown. The original church (seen below) was completed in 1871, designed by Jordan & Anderson, and was at first considered by parishioners to be too extravagant. Founding Pastor James Hennessey disagreed, prophesying that St. Patrick's would someday become the Cathedral of Detroit. He was proven correct almost 20 years later in 1890, when Bishop Foley designated that church on Adelaide as the diocesan cathedral. At that time it was also renamed Saints Peter & Paul Church, however. It reverted back to being regular St. Pat's in 1938 when the cathedral was changed to Most Blessed Sacrament on Woodward, and Detroit was designated as an archdiocese.
Image from DUCP
While St. Pat's served as the city's cathedral, they built a parochial school uptown on Parsons Street in 1892, named St. Therese School (seen below). The walk from school to mass for the students was eventually considered too dangerous as Detroit became more congested, so in 1926 they built a chapel next to it, the Chapel of St. Therese of the Little Flower (seen in the top photo).
St. Therese School closed in 1969, and in 1972 the rapidly shrinking St. Pat's parish moved into this smaller facility on Parsons Street; the Chapel of St. Therese of the Little Flower became the new St. Patrick's Church. One year later the former St. Therese School was reopened as the St. Patrick Senior Center and food pantry, to minister to the elderly of the Cass Corridor. They have also hosted the St. Patrick's Irish Festival here every June, a tradition that celebrated its 40th anniversary in 2017. The school was designed by local architect Leon Coquard:
Meanwhile, the old St. Pat's church on Adelaide had been sitting abandoned since 1983.
Photo by Mary Schroeder / Detroit Free Press
It finally burned down in 1993.
The entrance to the St. Therese / Patrick School is flanked by two rather extensive stone carvings.
As the St. Patrick Senior Center the building has been serving the senior citizens of the Cass Corridor for the past 45 years or so, ever since Sister Mary Watson opened the doors to cook a decent meal for a handful of needy old folks in 1973. The center now provides a wide range of services, activities, and classes for elderly people of all denominations, and boasts an outreach that extends to over 2,000 residents. I am surprised that many seniors citizens even remain in the Cass Corridor in light of the thorough regentrification of the area.
According to its website, St. Patrick Senior Center offers a comprehensive health and wellness program, a clinic, transportation assistance, as well as classes in art, technology, exercise and dancing, healthy living, and social activities. It sounds like everything a retirement community tries to be, but it's a 501c3 non-profit. The Detroit Area Agency on Aging even dubbed it a model for senior centers in the region.
The inside of the old parish school is beautiful, and centered around an old, intimate auditorium.
Here is where the bands play during the Irish Festival, kids and old folks dance on the dance floor, and I sit up in the balcony and drink Guinness. The attendees of the festival are an even mix of black and white, which seems odd at first since you don't usually find too many black Irish Catholics anywhere. But, as with many of these obscure Detroit things, we take all kinds.
The balcony creaks loudly with its antique wooden construction, and the chairs are probably c.1892 originals. This place is a total time capsule.
Incidentally the window in the 2nd floor men's room has a unique view of the sanctuary next-door...
The chapel here on Parsons was built in 1926, although it closed as a church in 2015. I think I heard that the Detroit Symphony Orchestra sometimes uses the chapel as a practice space, or once did a small concert or recording there.
"Oh, there you are!"
Now having gotten a bit of the barley in us, our mischievous streak inevitably began to take hold...
Pretty soon we found ourselves in the cavernous attic...because that's what we do, I guess.
Unimpressed with the large assemblage of rummage sale fodder being stored up here, I quickly turned my attention to the breezy attic window on this muggy summer day. I was pleasantly surprised by the view above the trees:
As I often do, I leaned further out and tried to get photos of this building's architectural details. Hey, there's gargoyles or something up there...
As I gazed up at these hidden little stone faces, I thought that they looked a hell of a lot like the grotesques at the entrance doors of Ste. Anne's Church. As it turns out, this school was designed by the same architect who designed Ste. Anne's, which explains why these look so familiar. He also designed the Soldier's Monument in Grand Rapids.
The rear of the Masonic Temple, and the Cass Plaza Apartments:
The Hotel Charlevoix and Hotel Park Avenue were still standing when I took these shots, and the ruins of the Scott Mansion had not been rebuilt yet:
Motor City Casino, Zug Island, King's Arms, etc:
The train station, before the fake windows:
Looking down Woodward towards Orchestra Place and the Bonstelle Theater:
I have a hunch that the history of the Chapel of St. Therese of the Little Flower is somehow connected to the famous/infamous Shrine of the Little Flower up at 12 Mile and Woodward in Royal Oak...they were both started the same year, and are both named after the same saint.
It's hilarious that for someone who can best be described as an agnostic ex-Catholic, I spend so much time at so many church festivals. I just like the buildings. And the beer tent.
In all seriousness, I do enjoy supporting the many historic church fundraisers in Detroit, whether it's the excellent fish fry or Pierogi Fest at Sweetest Heart of Mary, the German dinner at St. Joseph's, or the incredible music programs at Old St. Mary's, St. Paul's Cathedral, or Fort Street Presbyterian. Even St. Hyacinth has a Banana Festival that I've been meaning to check out...
Support your local historic church.
Catholic Churches of Detroit, by Roman Godzak, p. 32
Detroit's Historic Places of Worship, edited by Marla O. Collum, Barbara E. Krueger, Dorothy Kostuch, p. 237
"Empty Church Up In Flames," Detroit Free Press, May 5, 1993, p. 1
http://placepromo.com/DUCP/02/531-403-4.jpg
http://placepromo.com/DUCP/02/531-403-4b.jpg
http://placepromo.com/DUCP/07/parsons64.jpg
http://stpatsrctr.org/history0.aspx
http://detroitchurchblog.blogspot.com/2014/01/st-patrick-parish.html
https://www.shrinechurch.com/history-of-the-church/
Labels: Wayne County
Old Mack
If you follow Mack Avenue out across Detroit's east side just before Conner it goes up over the rail yard on a huge modern overpass at Chrysler's Mack Stamping / Budd Wheel Plant, but tucked off to the side there was a row of buildings that used to stand on Mack before the grade-separation was built. On today's maps it is called "Mack Service Road," but I've also seen it called "Old Mack." It's a dead-end road now, a stub cut off from its parent by the big overpass directing traffic elsewhere, leaving it to die.
Ruins from one collapsed building were spilling over into Manz Playfield:
As of 2018 most of these buildings have been demolished, so here is a brief run-down of some of their history.
The building on the right in the next photo still bears a date-stone in its cornice, reading "1919"...it was originally the Pitman & Dean Co. (coal & ice supply) at 12165-69 Mack. The sign under the FOR SALE sign says that it used to be the ____ Cold Extrusion Corp. It was occupied from at least 1977 to 1986 by lmerman Industries, Inc., who also did metal extrusion work, according to hits I found via Google Books.
...The building on the left was originally part of the J.A. MacIvory Lumber Co.'s Mack Avenue Yard. The c.1929 Sanborn map of this street shows the following other businesses here at that time: the McDonald Coal & Brick Co. Yard at 12017 Mack, the C.P. Steinheiser Co. (builders' supplies) at 12035 Mack, and the Grace Harbor Lumber Co. at 12081 Mack. None of them still stand.
Sadly, the c.1910 map does not cover this area, indicating that it was not developed land yet. This spot was still a couple hundred yards outside city limits in 1910, in what was then considered the Village of St. Clair Heights. This block would have been located right under the map key, across the tracks from the Lozier Motors plant:
Image of 1910 Sanborn map from loc.gov
The Lozier Motors plant once stood at 11801 Mack, a small luxury car company that was started in 1910 to rival Packard. According to the book How Detroit Became the Automotive Capital, Henry Ford and James Couzens visited Lozier Motors frequently to watch the assemblers working on the chassis line in the Albert Kahn-designed plant. Lozier fizzled out in 1915 when Cadillac essentially put them out of business. Their plant was bought by the Motor Products Corp.
Here is a snapshot of the area in 1929...we are standing right under the number "61" at center:
The vacant patch where 55 is used to be a Hudson Motors factory. Across the street on the south side of Mack from us there was mostly empty space in 1929, behind the Budd Wheel and Hudson Motors plants...which were later turned into Chrysler's Mack Stamping Plant.
On a later second visit to this street I found there to be massive damage done since I was here last…scrappers got at it. In fact, they were there while we were there.
Talk about wrack & ruin...Edison poles chopped down and the whole bit. Keep in mind, this is mid-2009 near the height of the scrapping epidemic. After my first visit, the remnants of this street spiraled very rapidly into complete dissolution.
So much for the roof…scrappers "Packardized" that one (ripped out the iron trusses and let it fall). It looks like that is what's getting ready to happen here too, with the iron posts exposed and ready to be notched with a cutting torch, just like lumberjacks felling a tree:
I believe I remember hearing that at least one of these structures was set ablaze too. A cell tower site sits in the middle of the ruins:
More missing roof trusses:
Whoops, bit of a flood here...
The blue paint mark "W/O" in the next photo means that the water has been shut off to the building by the city (probably after the pipe froze and burst, causing that flood in the photo above):
This yellow building, at 12121 Mack, was the Foam Distributing Co., at least according to the sign on the front of the building, and a reference to them in a 1997 business directory.
That grey stone building on the far end, at 12101 Mack (which I now regret not going into), used to be the UAW Local 212 union hall. Here it is on Google Streetview, in 2013:
Image via Google Streetview
It was also the location of a popular barn dance every Saturday night...the heart of industrial Detroit seems a weird place to find a shindig, but according to a couple books I searched online, this building was sort of like a country equivalent of the Grande Ballroom on weekends. Local bluegrass pioneer Cranford "Ford" Nix was a member of Local 212 and helped Casey Clark secure the hall for his dances. Besides hosting the "Lazy Ranch Barn Dance" here Casey Clark was a fiddle player who even had his own TV show on CKLW-TV, and deejayed a country show on WJR radio in the 1950s, according to The Birth of the Detroit Sound: 1940-1964.
It probably sounds weird to think that Detroit ever had a country music scene of all things, but don't forget that in the Postwar, post-Depression era, Detroit was flooded by an influx of poor Appalachians looking for work in the factories, and they certainly brought their banjos and fiddles with them. Ford Nix himself worked at the old Chrysler plant here on Mack Avenue. Local 212 was the biggest and strongest UAW local on the east side back in those days, and they represented the Briggs Mfg. plants around here, which were the scene of several major battles in Detroit's organized labor movement.
This Google Streetview image (above) from October of 2011 shows that like many buildings in Detroit during the Great Recession someone painted "NO COPPER" on the front entrance when it was boarded up, to indicate to would-be scrappers that all the valuable metal had already been removed, in hopes that it would spare the building from being ripped open. Little did they know, skyrocketing metal prices would soon lead the scrappers to come for the actual iron structural members of the buildings.
Since learning all this history about the humble little building at the end of a dead-end street, I decided to pay another quick visit in early 2019 so I could actually go inside. I was surprised to find a somewhat decorative entryway (above).
Once inside it looks like there was a small bar here, which is strange because I know that no UAW members ever drink any alcoholic beverages at all! ;)
These three doors led into the large gathering space in the rear of the building, which is collapsed:
I imagine that this is where the old union meetings and "Lazy Ranch Barn Dances" used to be held, back when Detroit had about a million more people living here.
Sanborn map for Detroit, Vol. 19, Sheet 61, etc. (1929)
Sanborn map for Detroit, Vol. 8, Sheet 95 (1910)
How Detroit Became the Automotive Capital, by R. Szudarek
Automotive Engineering, Volume 86, p. 149
Michigan Manufacturer's Directory, (1997), p. 139
The Birth of the Detroit Sound: 1940-1964, by Marilyn Bond and S.R Boland, p. 33
Detroit Country Music: Mountaineers, Cowboys, and Rockabillies, by Craig Maki, Keith Cady, p. 307
American Directory of Organized Labor (1992), p. 528
https://www.peoplesworld.org/article/the-uaw-212-cio-flying-squad-comes-back-to-life-one-afternoon/
https://deepblue.lib.umich.edu/handle/2027.42/128556
Labels: UAW Local 212 Hall, Wayne County
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Designed and optimized for athletes seeking an unobstructed field of view and maximum ventilation.
The SL-1 offers every athlete the perfect fit courtesy of the adjustable titanium core wire design. Patented GEKO™ technology provides unparalleled retention on the roughest of courses. With our world-class C3™ lenses and lens coatings and simple lens interchangeability with lock-tab security, the SL-1 delivers an uncompromising sport frame for racing, training, and everything in between. Weighing in at only 22gm, the SL-1 is lighter, faster, and more technologically advanced than any rimless shield on the market.
Optimized for road cycling, this is an extremely versatile high-contrast lens that also offers significant infrared protection. Designed for partly cloudy to bright and sunny conditions, this lens also performs excellently on the trail.
Optimized for road cycling, this lens provides significant contrast and comfortability while enhancing the white lines on the road and traffic lights for all-around safety. Designed for partly cloudy to sunny conditions.
Critical performance coatings include front and backside hydro/oleophobic coatings to keep moisture of any kind from sticking on the lens; front and back-side anti-scratch protection; a multi-layer anti-reflective back-side coating; an anti-fog Ri-Pel™ coating on the back of the lens; and a multi-layer mirror coating or polarization film.
The SL-1 comes fitted with customizable titanium core wires that offer ultralight stability while also allowing the wearer to adjust the temple pieces for a precision fit. Wrapped in GEKO™, the core wire fit system ensures unmatched security, retention and comfort for every athlete.
Featuring GEKO™ technology, the nose piece locks down the fit and security of the frame. Additionally, it is easily removable for lens cleaning or a quick color swap with another accessory color.
The lens is easily removable and interchangeable with additional ROKA SL-1 accessory options to meet the needs of every run, ride, or race. The lens lock tab provides a simple guide for placement and peace of mind knowing your lens is securely seated.
Design evolved over a billion years. Inspired by the soft but amazingly sticky feet of the Gecko, our patented GEKO™ fit and retention system features a proprietary elastomer for nose and temple pads that's hydrophilic, chemical resistant and supports multi-directional traction with comfort.